arXiv:1602.01336v2 [astro-ph.SR] 8 Feb 2016 cp tClrAt bevtr CH) n h . m 4.2 the and (CAHA), Observatory Alto Tele- Calar m 3.5 at the Tele- scope (LCO), Pont Observatory du Campanas m Ob- Las 2.5 at the the scope at (OSN), Telescope Nevada m Sierra 1.5 de the servatorio facilities: five with gathered et fAtooy nvriyo lrd,21Byn Space Bryant 211 Florida, of University Astronomy, of Dept. etod srboo´a SCIT,cmu SC aiob camino ESAC, campus Astrobiolog´ıa, CSIC-INTA, de Centro nttt eAto´sc eL lt CNCT NP,Pase UNLP), (CONICET, Plata La Astrof´ısica de de Instituto nv eea oRoGad oNre-UR,CiaPsa 1524 Postal Caixa UFRN, - Norte do Grande Rio do Federal Univ. FSS P,Uiesddd lcne artr a Vicent San carretera Alicante, de Universidad EPS, DFISTS, FSS P,Uiesddd lcne artr a Vicent San carretera Alicante, de Universidad EPS, DFISTS, 1 nttt eAto´sc eAdlcı-SC lreade Andaluc´ıa-CSIC, Astrof´ısica Glorieta de de Instituto nttt eAto´sc eAdlcı-SC lreade Andaluc´ıa-CSIC, Astrof´ısica Glorieta de de Instituto h OS pcrsoi aai hsatcewere article this in data spectroscopic GOSSS The eatmnod ´sc,Uiesddd aSrn,A.Cist Av. Serena, La de F´ısica, Universidad de Departamento ae nnwhmgnos ihsga-onieratio, signal-to-noise high homogeneous, new on based nteps,itoueteueo uioiycasI tseta typ spectral (2016). at al. et IV headings: Arias class Subject of luminosity work of the use to the scheme e classification introduce stars past, of examples the ide O egregious in also of also some We We 5 present and type. stars. classifications, O+O+B type O of GOSSS O+O (SB3) new of binary are 20 spectroscopic 6 tripled-lined are which new there of objects (SB2s), syst binaries new O-type spectroscopic the of Among total the a 590. bringing 142 to hemispheres, present we both paper from this stars In O (GOSC). Catalog O-Star Galactic the surveys — eatmnod srfıia nvria eL aua E- Laguna, La de Astrof´ısica, Universidad de Departamento eatmnod srfıia nvria eL aua E- Laguna, La de Astrof´ısica, Universidad de Departamento hsi h hr ntlmn fGSS asv pcrsoi surve spectroscopic massive a GOSSS, of installment third the is This pc eecp cec nttt,30 a atnDie B Drive, Martin San 3700 Institute, Science Telescope Space h aatcOSa pcrsoi uvy(GOSSS). Survey Spectroscopic O-Star Galactic The nttt eAto´sc eCnra,E3 0 aLgn,T Laguna, La 200 E-38 Canarias, Astrof´ısica de de Instituto nttt eAto´sc eCnra,E3 0 aLgn,T Laguna, La 200 E-38 Canarias, Astrof´ısica de de Instituto iaissetocpc—bnre:iul—saseryt stars:early — binaries:visual — binaries:spectroscopic I.12adtoa -yesystems O-type additional 142 III. .I ra,R .Barb´a H. R. Arias, I. J. .Ma´ız Apell´anizJ. .R Walborn R. N. ABSTRACT .Sim´on-D´ıazS. .Negueruela I. .C Gamen C. R. .R .Le˜ao S. R. J. .J Alfaro J. E. .Sota A. .Herrero A. .Marco A. 1 2 , 3 cpoCnra GC tOsraoi e ou elos de Roque del Observatorio (ORM). at Tele-Muchachos Gran (GTC) m Canarias 10.4 scopio and (WHT) Telescope Herschel William , 4 R aAtoo´asn -808Gaaa Spain Granada, 008 E-18 Astronom´ıa s/n, la aAtoo´asn -808Gaaa Spain Granada, 008 E-18 Astronom´ıa s/n, la 3 2 2 iiigAtooe,CH,Spain. CAHA, Astronomer, Visiting Chile. LCO, Astronomer, Visiting ∼ , cec etr ansil,F 261 USA 611, 32 FL Gainesville, Center, Science 3 e api /,E0 9 lcne Spain Alicante, 690 E-03 s/n, Raspeig del e e api /,E0 9 lcne Spain Alicante, 690 E-03 s/n, Raspeig del e e oqesn 90L lt,Argentina Plata, La 1900 s/n, Bosque del o j e atlosn -862Mdi,Spain Madrid, 692 E-28 s/n, castillo del ajo , 50dgtlosrain eetdfrom selected observations digital 2500 4 , 5 ra 20Nre aSrn,Chile Serena, La Norte, 1200 ernas 825L aua eeie Spain Tenerife, Laguna, La 205 38 825L aua eeie Spain Tenerife, Laguna, La 205 38 2 E 90890 aa N Brazil RN, - Natal 078-970, 59 CEP , m ulse ihnteproject the within published ems lioe D2 1,USA 218, 21 MD altimore, rnosycasfida O-type as classified rroneously dtoa tla ytm with systems stellar dditional Btp,ada additional an and type, +B sO-55 n dp the adapt and O4-O5.5, es p tr:msinline,Be stars:emission — ype eiesm fteprevious the of some revise tf 1nwdouble-lined new 11 ntify nrf,Spain enerife, nrf,Spain enerife, fGlci stars, O Galactic of y 1 1. Introduction graph at the Las Campanas (LCO) 2.5 m du Pont telescope). Starting with paper II, some spec- The Galactic O-Star Spectroscopic Survey tra were also obtained with the ISIS spectrograph (GOSSS) is a long-term project that is obtain- at the 4.2 m William Herschel Telescope (WHT) ing homogeneous, high SNR, R ∼ 2500, blue- at the Observatorio del Roque de los Muchachos violet spectra of a large number (1000+) of (ORM) in La Palma, Spain. In this paper we use O stars in the Milky Way and deriving accu- data from all of the above instruments and we also rate and self-consistent spectral types for all of add a new one, OSIRIS, at the 10.4 m Gran Tele- them (Ma´ızApell´aniz et al. 2011). In Sota et al. scopio Canarias (GTC) at the ORM (Table 1). (2011), from now on paper I, we presented the Only a few GTC spectra are used here but the first installment of the survey, which was com- ◦ number will increase in future GOSSS papers, as prised of the results for 178 northern (δ > −20 ) we have already acquired data for over 200 stars, O stars. In Sota et al. (2014), from now on paper most of them too dim to be accessible with the II, we extended the sample to the southern hemi- other telescopes mentioned above. One difference sphere for a total of 448 O stars. Papers I and between the GTC setup and the rest is that we use II concentrated on the brightest O stars with the two volume-phased holographic gratings, R2500U aim of achieving completeness down to B = 8 but and R2500V, allowing us to cover a larger wave- they also included many dimmer stars. This third length range than with the other instruments. The paper continues the previous work by adding 142 exposures for the two gratings are taken consecu- new stars and raising the sample size to 590. Most tively, with the time difference between the first of the new stars are of luminosity class V, which one and the last one being always less than one are relevant to the OVz phenomenon (Arias et al. hour in order to avoid changes in the phase of 2016), but objects of other luminosity classes are rapidly moving spectroscopic binaries. As we do also included. with the rest of the spectrographs, we use checks This paper is organized as follows. We first to compare that the quality of the data from all present the changes in the observational setup and the spectrographs is uniform and, in those cases the classification scheme in section 2. Then, the where the spectral resolution is higher than 2500, spectral classifications are shown in section 3, di- we degrade it to that value. vided in updates to O stars present in papers I We have also started taking GOSSS data with and II, new O stars, and late-type stars previously [a] the GMOS spectrograph at the 8.1 m Gemini misclassified as of O type. Finally, in section 4 we South telescope, [b] the Goodman High Through- analyze the status of the project based on the new put Spectrograph at the 4.1 m SOAR Telescope spectral classifications. (both at Cerro Pach´on, Chile), and [c] FRO- DOspec at the 2.0 m Liverpool Telescope (at the 2. Data and methods ORM) but we do not use them in this paper; their first GOSSS spectra will likely appear in a future 2.1. Blue-violet spectroscopy with R ∼ 2500 paper IV. The GOSSS data were described in papers I and The GOSSS data in this paper were obtained II and the reader is referred there for further in- between 2007 and 2015. The OSN and LCO ob- formation. Here we detail the changes from those servations were obtained in visitor mode, the GTC previous works. observations in service mode, and the CAHA ob- Most of the spectra presented in paper I were servations in a combination of both. For some SB2 obtained with the Albireo (Observatorio de Sierra and SB3 spectroscopic binaries, multiple epochs Nevada - OSN - 1.5 m telescope) and TWIN (Calar were obtained to observe the different orbit phases. Alto - CAHA - 3.5 m telescope) spectrographs. On In cases with known orbits, observations near the other hand, most of the spectra in paper II quadrature were attempted. were obtained with the Boller & Chivens spectro- The spectral classifications which are the main content of this paper are presented in Ta- 4 Visiting Astronomer, WHT, Spain. bles 4, 5, and 6 and they were obtained with MGB 5 e-mail contact: [email protected]. Ma´ızApell´aniz et al. (2012, 2015c).

2 Table 1: Telescopes, instruments, and settings used in this paper.

Telescope Spectrograph Grating Spectral scale Spatial scale Wav. range (A/px)˚ (′′/px) (A)˚ LCO 2.5 m (du Pont) Boller & Chivens 1200 0.80 0.71 3900−5500 OSN 1.5 m Albireo 1800 0.62 0.83 3750−5070 CAHA 3.5 m TWIN (blue arm) 1200 0.55 0.58 3930−5020 ORM 4.2 m (WHT) ISIS (blue arm) 600 0.44 0.20 3900−5600 ORM10.4m(GTC) OSIRIS 2500U 0.62 0.25 3440−4610 2500V 0.80 0.25 4500−6000

2.2. Cataloguing 2.3. Spectral classification methodology and the new standard grid The spectral types are available through the lat- est version (currently v3.2) of the Galactic O-Star The spectral classification methodology was Catalog (GOSC, Ma´ızApell´aniz et al. 2004), ac- laid out in paper I and some changes were pre- cessible at http://gosc.iaa.es. Starting in ver- sented in paper II. Here we introduce two addi- sion 3, the GOSSS spectral types are the default tional changes. ones and the basis for the catalog selection, though The first one concerns the OVz phenomenon, older classifications and those obtained with high- described in detail in Sab´ın-Sanjuli´an et al. (2014) resolution spectra are also kept as possible addi- and Arias et al. (2016). OVz stars have deep tional columns. B- and J-band photometry are He ii λ4686 absorption lines, likely caused primar- 1 also provided in GOSC for all stars . The rec- ily by their extreme youth, though additional fac- tified GOSSS spectra can also be obtained from tors may also play a role. In paper II, we defined GOSC as FITS tables. the z ratio as: The previous version of GOSC (3.1.2) had only entries in the main catalog, the part cor- EW(He ii λ4686) responding to O stars. Versions 2.0-2.4 of GOSC z = (Sota et al. 2008) did include four supplements for Max[EW(He i λ4471), EW(He ii λ4542)] WR and WR+O systems, other early-type stars, (1) late-type stars, and extragalactic massive stars, by measuring the equivalent widths of He i λ4471, respectively. Since here we are presenting some He ii λ4542, and He ii λ4686 in our main-sequence late-type stars (see below), we are reintroducing standard stars and classified a star as OVz when the third supplement in GOSC 3.2. In future pa- z was greater than ∼ 1.0. Arias et al. (2016) an- pers, we plan to release GOSSS spectral types for alyzed the OVz phenomenon and decided to raise the other three supplements and we will populate the critical value of z to 1.1 to avoid the borderline, GOSC accordingly. often unclear, cases. Here we adopt that criterion The GOSSS spectral types were first made and reclassify some of the stars in papers I and II. available at GOSC in June 2013 as part of GOSSS The second one concerns the range of spec- Data Release 1.0 (GOSSS-DR1.0, Sota et al. tral types for which luminosity class IV is defined. 2013). Later changes led to Data Releases 1.1 When the O-type luminosity classification was in- (with the spectral types from Sota et al. 2014) and troduced and calibrated by Walborn (1971, 1972, 1.1.1 (minor changes in August 2014). The addi- 1973) only three classes (V, III, I) were defined tion of new spectral types and changes to previous for spectral types earlier than O6. The luminos- ones presented here constitutes GOSSS-DR2.0. ity range is relatively small at those types, and there was concern about possible differences in the 1 See Ma´ız Apell´aniz et al. (2013) for details, we use Bap and strong stellar winds unrelated to luminosity affect- Jap, respectively, to refer to the photometry in GOSC, ing the Of criteria at the earliest types. Neverthe- where “ap” refers to approximate and is intended to be significant only to one tenth of a magnitude. less, bright giants (class II) and supergiant subcat-

3 egories (Ia, Iab, and Ib) were defined as early as the grid filled with respect to the previous version. types O6-O6.5, while Sota et al. (2011) extended We plan to keep filling those gaps when we find ad- the use of class IV as well to those types in the ditional appropriate stars within our survey. Note larger, higher quality GOSSS sample. It is also that most of the gaps occur at the earliest types relevant that subsequent UV work demonstrated (O5.5 and earlier for the III to Vz columns, O7.5 a high degree of correlation (and, by implication, and earlier for the supergiants), which is expected robustness) between the stellar-wind profiles and given the scarcity of those types in the solar neigh- the optical spectral types throughout the entire borhood. One possibility we will consider in the O-type range (Walborn et al. 1985). future is the use of LMC O stars. In the context of the quantification of the z ra- tio by Arias et al. (2016), we have become aware 3. Results of several spectra classified as type V with exces- This section constitutes the main body of the sively small values of the ratio, i.e. in the range paper, the spectral classifications, and is divided 0.5-0.7. A number of them are of types O4-O5.5, in three parts. First, we revise some of the re- and inspection from this viewpoint reveals Of mor- sults from papers I and II. Second, we present new phologies in the GOSSS data well intermediate be- spectral classifications for O stars not included in tween most class V spectra and the class III stan- those papers. Third, we show some cases previ- dards, in terms of both the He ii λ4686 absorption ously classified in the literature or in Simbad as and N iii λ4634-41-42 emission strengths. Multi- being O stars which turn out to be of late type. ple observations of several of these spectra demon- The information is given in Tables 4, 5, and 6, with strate robustness in these features. Hence we now details about each star (sorted by GOS ID within define luminosity class IV at types O4-O5.5 to de- each subsection) provided in the text. scribe such spectra. In view of the strengths of the Of features in most of them, we adopt the 3.1. Stellar systems from papers I and II (f)-parameter for them, as opposed to ((f)) for class IV at types O6 and later. We also note that 3.1.1. Name changes due to the discovery of HD 93 250 AB was previously assigned to class III companions by Sota et al. (2014), whereas it is clearly more In the last two years, several papers have used similar to the other class IV objects; originally it high-spatial resolution techniques to detect new had been classified as V. Thus, this classification bright visual close companions to stars present in enhancement improves the consistency of the lu- papers I and II. The proximity of those compan- minosity classification at these types. ions (with separations of tens of miliarcseconds or Calibration work to determine whether this less) do not allow us to obtain separate GOSSS classification development corresponds to a con- spectra for them but the nomenclature used in sistent luminosity difference remains for the fu- GOSSS (a companion must be included in the ture, likely depending upon Gaia (Perryman et al. star name if it contributes a significant fraction 2001) measurements for reliable results. However, of light to the blue-violet spectrum, established as regardless of how that turns out, the development ∆B ≤ 2.0) makes us change the name of the star provides a more precise systematic description of from the one listed in our previous papers. The the spectra themselves. name changes are given in Table 3, where no spec- The two changes above (the critical value for tral types are listed since they remain unchanged the OVz phenomenon and the definition of lu- unless the system is also listed in the next subsub- minosity class IV for O4-O5.5 stars) imply up- section. Table 3 gives the current GOSSS name dates on the standard grid used for spectral clas- (with all the currently known bright components sification. The first GOSSS-based standard grid included in the Washington Double Star Catalog, (OB2500 v1.0) was presented in Sota et al. (2011) WDS, Mason et al. 2001), the GOSSS ID, the ref- and the second one (OB2500 v2.0), which filled erence, the new component, and possibly a com- some gaps, in Ma´ızApell´aniz et al. (2015c). Here ment. Note that most of the new components are we present OB2500 v3.0 in Table 2, with an addi- from Sana et al. (2014). tional column for OVz standards and some gaps in

4 Table 2: The OB2500 v3.0 grid of classification standards.

Vz V IV III II Ib Iab/I Ia O2 HD 93 129 AaAb O3 HD 64 568 · · · · · · Cyg OB2-7 O3.5 HD 93 128 · · · Pismis 24-17 NGC 3603 HST-48 O4 HD 96 715 HD 46 223 HD 168 076 AB · · · HD 15 570 HD 93 250 AB HD 16 691 HD 190 429 A O4.5 · · · HD 15 629 HD 193 682 · · · HD 14 947 HDE 303 308 AB Cyg OB2-9 O5 HD 46 150 HDE 319 699 HD 168 112 AB HD 93 843 CPD -47 2963 AB O5.5 · · · HD 93 204 ··· ··· Cyg OB2-11 ALS 18 747 O6 HD 42 088 ALS 4880 HD 101 190 AaAb HDE 338 931 HDE 229 196 ··· ··· HD 169 582 HDE 303 311 CPD -59 2600 O6.5 HD 91 572 HD 167 633 HDE 322 417 HD 190 864 HD 157 857 ··· ··· HD 163 758 HD 12 993 HD 96 946 HD 152 723 AaAb HD 156 738 AB O7 HD 97 966 HD 93 146 A ALS12320 CygOB2-4A HD 94 963 HD 69 464 ··· ··· CPD -58 2620 HD 93 222 AB HD 93 160 AB HD 151 515 HD 193 514 HDE 242 926 HD 91 824 O7.5 HD 152 590 HD 35 619 HD 97 319 HD 163 800 HD 34 656 HD 17 603 HD 192 639 · · · HD 171 589 HD 156 154 9 Sge O8 HDE 305 539 HD 101 223 HD 94 024 HDE 319 702 63 Oph BD -11 4586 HD 225 160 HD 151 804 HDE 305 438 HD 97 848 HD 135 591 λ Ori A HD 191 978 O8.5 HDE 298 429 HD 46 966 AaAb HD 114 737 AB HD 75 211 HD 125 241 · · · HDE 303 492 HD 14 633 AaAb HD 218 195 A HD 207 198 HD 46 149 HD 57 236 Trumpler 14-9 O9 10 Lac HD 93 028 HD 93 249 A HD 71 304 19 Cep HD 202 124 α Cam HD 216 898 CPD -41 7733 HD 24 431 τ CMa AaAb HD 152 249 CPD -59 2551 HD 210 809 O9.2 HD 46 202 HD 96 622 CPD -35 2105 AaAbB ALS 11 761 HD 76 968 HD 154 368 HD 152 424 HD 12 323 HD 16 832 HD 123 008 HD 218 915 O9.5 AE Aur HD 192 001 HD 96 264 δ Ori AaAb · · · HD 188 209 · · · µ Col HD 93 027 HD 155 889 AB O9.7 υ Ori HD 207 538 HD 189 957 HD 68 450 HD 47 432 HD 225 146 HD 195 592 HD 154 643 HD 152 405 HD 154 811 µ Nor GS Mus HD 10 125 HD 152 147 HD 104 565 HD 191 781 ◦ ◦ Notes Normal, italic, and bold typefaces are used for stars with δ > +20 , δ < −20 , and the equatorial intermediate region, respectively.

5 3.1.2. Spectral type changes HD 173010 = BD -09 4805 = ALS 9901. This object was classified as O9.7 Ia. Walborn et al. In Table 4 we list the stellar systems already (2016) changed the luminosity class to Ia+ based included in papers I and II for which we have ob- on GOSSS data. tained revised spectral types. They are ordered by GOSSS ID, which corresponds for practical pur- poses to an ordering by Galactic longitude l2 The HD 192281 = V2011 Cyg = ALS 10943. corresponding spectrograms are shown in the same This object is one of the new O4-O5.5 IV stars. order in Fig. 1. The majority of the systems in this section are included because of a change in the z HDE 229232 AB = BD +38 4070 AB = suffix, as described in subsection 2.3. A minor- ALS 11296 AB. This object has anomalous ity are included due to the definition of luminos- and broad line profiles, possibly originating in ity class IV for types O4-O5.5 (see subsection 2.3) a companion. Note that Aldoretta et al. (2015) or the assignment of an SB2 status to the sys- found a bright companion which is spatially unre- tem in the GOSSS data that was not possible at solved in the GOSSS data, hence the AB compo- the time of papers I and II. Since all of these sys- nent designation. Williams et al. (2013) identify tems have been already discussed in the previous this system as an SB1 with a preliminary period GOSSS papers, we only present additional details of 6.2 d. about some of them in this section. In particular, The ((f)) suffix for this object was omitted by we discuss several SB2 systems for which we have mistake in paper II. fine-tuned the spectral classification using the new standard grid. HD 14434 = ALS 7124. This star is one of the new O4-O5.5 IV stars. HD 165052 = ALS 4635. We have obtained observations at a new epoch for this SB2 that has allowed us to improve the classification of HD 48099 = ALS 9098. We have reana- O5.5: Vz + O8: V of paper II to O6 Vz + O8 Vz. lyzed the data for this SB2 to change the clas- The system was caught at a velocity separation sification of O5 V((f))z + O9: V of paper II to ∆v between the two spectroscopic components of O5.5 V((f))z + O9 V. The system was caught at ∼200 km/s. a ∆v of ∼140 km/s.

HD 168075 = NGC 6611-197. We have ob- HD 92206 C = CPD -57 3580 = ALS 1695. tained observations at a new epoch for this star We have reanalyzed the data for this SB2 to and derived a spectral type of O6.5 V((f)), slightly change the classification of O8 Vz + O9.7 V of earlier than the one in paper I. The change is not paper II to O8 V(n)z + B0: V. The system was surprising, given that this object is an SB2 classi- caught at a ∆v of ∼425 km/s. fied as O6.5 V((f)) + B0-1 V by Sana et al. (2009). ALS 15204 = CPD -56 2608 A = Trum- HD 168076 AB = ALS 4908 AB. This sys- pler 14 MJ 92. In paper II we identified this tem is one of the luminosity class IV standards object as an O star for the first time and we hinted due to the introduction of that class for the spec- it may be an SB2. For this paper we obtained tral subtypes O4-O5.5. a new epoch and we indeed detect it is an SB2 caught with a ∆v of ∼150 km/s (which is a low separation for GOSSS but it is possible because HD 168112 AB = ALS 4912 AB. This star of the small magnitude difference between the two is one of the luminosity class IV standards due components and their low v sin i). The GOSSS to the introduction of that class for the spectral spectral classification is O7.5 Vz + O9: V. We also subtypes O4-O5.5. placed ALS 15203 (= CPD -56 2608 B), located 4′′. 8 away, on the slit and found it is an early-B 2 The only exceptions being systems with very similar values star. of l.

6 i.1—Setorm o tr led rsn nppr n II and I papers in present already stars for Spectrograms 1.— Fig. 0.0 0.5 1.0 1.5 2.0 2.5 3.0 3.5 4.0

ε 0045 504750 4500 4250 4000 H

He I 4009 He I+II 4026

N IV 4058 C III 4068 / 69 / 70 Si IV 4089 Hδ N III 4097 Si IV 4116 He I 4121 HD 173010O9.7Ia+var HD 168112ABO5IV(f) HD 168076ABO4IV(f) HD 168075O6.5V((f)) HD 165052O6Vz+O8 9 SgrABO4V((f)) HD 164536O7.5V(n) He I 4144

He I 4169 DIB is 4179 C III 4187 He II 4200

DIB is 4273

Hγ Wavelength (Å) N III 4379 He I 4388 7 DIB is 4428 He I 4438

He I 4471

DIB is 4502 N III 4511 / 15

He II 4542

h agt r otdb O ID. GOS by sorted are targets The . Si III 4553 Si III 4568 / 75 DIB is 4591 N V 4604 / 20 Si IV 4631 N III 4634 / 41 / 42 Si IV 4654 C III 4647 / 50 / 51

He II 4686

He I 4713 DIB is 4727

DIB is 4762 / 65 / 80

Si III 4813 / 20 / 29

Hβ DIB is 4880 / 87 N III 4905 He I 4922 i.1—(continued). 1.— Fig. 0.0 0.5 1.0 1.5 2.0 2.5 3.0 3.5 4.0

ε 0045 504750 4500 4250 4000 H

He I 4009 He I+II 4026

N IV 4058 C III 4068 / 69 / 70 Si IV 4089 Hδ N III 4097 Si IV 4116 He I 4121 HD 17520AO8V HD 14434O5.5IVnn(f)p BD +60513O7Vn HD 207198O8.5II((f)) HD 191978O8V HDE 229232ABO4V:n((f)) HD 192281O4.5IV(n)(f) HDE 344784AO6.5V((f))z He I 4144

He I 4169 DIB is 4179 C III 4187 He II 4200

DIB is 4273

Hγ Wavelength (Å) N III 4379 He I 4388 8 DIB is 4428 He I 4438

He I 4471

DIB is 4502 N III 4511 / 15

He II 4542 Si III 4553 Si III 4568 / 75 DIB is 4591 N V 4604 / 20 Si IV 4631 N III 4634 / 41 / 42 Si IV 4654 C III 4647 / 50 / 51

He II 4686

He I 4713 DIB is 4727

DIB is 4762 / 65 / 80

Si III 4813 / 20 / 29

Hβ DIB is 4880 / 87 N III 4905 He I 4922 i.1—(continued). 1.— Fig. 0.0 0.5 1.0 1.5 2.0 2.5 3.0 3.5 4.0

ε 0045 504750 4500 4250 4000 H

He I 4009 He I+II 4026

N IV 4058 C III 4068 / 69 / 70 Si IV 4089 Hδ N III 4097 Si IV 4116 He I 4121 CPD HD 64315ABO5.5V+O7 HD 48279AO8.5VNstrvar? HD 46485O7V((f))nvar? HD 48099O5.5V((f))z+O9V HD 36879O7V(n)((f)) HD 35619O7.5V((f)) HD 92206BO6V((f)) He I 4144 −

47 2962O7V((f)) He I 4169 DIB is 4179 C III 4187 He II 4200

DIB is 4273

Hγ Wavelength (Å) N III 4379 He I 4388 9 DIB is 4428 He I 4438

He I 4471

DIB is 4502 N III 4511 / 15

He II 4542 Si III 4553 Si III 4568 / 75 DIB is 4591 N V 4604 / 20 Si IV 4631 N III 4634 / 41 / 42 Si IV 4654 C III 4647 / 50 / 51

He II 4686

He I 4713 DIB is 4727

DIB is 4762 / 65 / 80

Si III 4813 / 20 / 29

Hβ DIB is 4880 / 87 N III 4905 He I 4922 i.1—(continued). 1.— Fig. 0.0 0.5 1.0 1.5 2.0 2.5 3.0 3.5 4.0

ε 0045 504750 4500 4250 4000 H

He I 4009 He I+II 4026

N IV 4058 C III 4068 / 69 / 70 Si IV 4089 Hδ N III 4097 Si IV 4116 He I 4121 CPD V572 CarO7.5V(n)+B0 HD 93250ABO4IV(fc) HD 93129BO3.5V((f))z ALS 15204O7.5Vz+O9:V HD 92206CO8V(n)z+B0:V CPD HD 93343O8V He I 4144 − − 59 2591O8Vz+B0.5:V: 59 2626ABO7.5V(n) He I 4169 DIB is 4179 C III 4187 He II 4200

DIB is 4273

Hγ Wavelength (Å) N III 4379 He I 4388 10 DIB is 4428 He I 4438

He I 4471

DIB is 4502 N III 4511 / 15

He II 4542 Si III 4553 Si III 4568 / 75 DIB is 4591 N V 4604 / 20 Si IV 4631 N III 4634 / 41 / 42 Si IV 4654 C III 4647 / 50 / 51

He II 4686

He I 4713 DIB is 4727

DIB is 4762 / 65 / 80

Si III 4813 / 20 / 29

Hβ DIB is 4880 / 87 N III 4905 He I 4922 i.1—(continued). 1.— Fig. 0.0 0.5 1.0 1.5 2.0 2.5 3.0 3.5 4.0

ε 0045 504750 4500 4250 4000 H

He I 4009 He I+II 4026

N IV 4058 C III 4068 / 69 / 70 Si IV 4089 Hδ N III 4097 Si IV 4116 He I 4121 CPD δ TU MusO8V(n)+B0 HDE 305525O5.5V((f))z+O7.5VB HD 93222ABO7V((f)) V662 CarO5V(n)z+B0:V HD 93146AO7V((f)) V1034 ScoO9.2IV+B1:V CirAaAbAcO7IV((f))+B He I 4144 −

41 7721AO9.7V:(n) He I 4169 DIB is 4179 C III 4187 He II 4200

DIB is 4273

Hγ Wavelength (Å) N III 4379 He I 4388 11 DIB is 4428 He I 4438

He I 4471

DIB is 4502 N III 4511 / 15

He II 4542 Si III 4553 Si III 4568 / 75 DIB is 4591 N V 4604 / 20 Si IV 4631 N III 4634 / 41 / 42 Si IV 4654 C III 4647 / 50 / 51

He II 4686

He I 4713 DIB is 4727

DIB is 4762 / 65 / 80

Si III 4813 / 20 / 29

Hβ DIB is 4880 / 87 N III 4905 He I 4922 i.1—(continued). 1.— Fig. 0.0 0.5 1.0 1.5 2.0 2.5 3.0 3.5

ε 0045 504750 4500 4250 4000 H

He I 4009 He I+II 4026

N IV 4058 C III 4068 / 69 / 70 Si IV 4089 Hδ N III 4097 Si IV 4116 He I 4121 HD 158186O9.2V+B1: HD 155806ABO7.5V((f))(e) HDE 319703AO7V((f))+O9.5V ALS 18770O7V((f)) HD 156292O9.7III+B HD 152623AaAbBO7V(n)((f)) He I 4144

He I 4169 DIB is 4179 C III 4187 He II 4200

DIB is 4273

Hγ Wavelength (Å) N III 4379 He I 4388 12 DIB is 4428 He I 4438

He I 4471

DIB is 4502 N III 4511 / 15

He II 4542 Si III 4553 Si III 4568 / 75 DIB is 4591 N V 4604 / 20 Si IV 4631 N III 4634 / 41 / 42 Si IV 4654 C III 4647 / 50 / 51

He II 4686

He I 4713 DIB is 4727

DIB is 4762 / 65 / 80

Si III 4813 / 20 / 29

Hβ DIB is 4880 / 87 N III 4905 He I 4922 HD 93250 AB = ALS 1859 AB. This object writing) while Ac is the third outer component is one of the new O4-O5.5 IV stars. resolved by Sana et al. (2014) with a period of 1644 d measured by Mayer et al. (2014). CPD -59 2591 = Trumpler 16-21 = ALS 15217. We have reanalyzed the data for this SB2 to V1034 Sco = CPD -41 7742 = ALS 15757. change the classification of O8.5 V + B0.5: V: In paper II we did not detect double lines in this of paper II to O8 Vz + B0.5: V:. The system was object in the GOSSS spectra, even though it is caught at a ∆v of ∼200 km/s. an SB2 system classified by Sana et al. (2008) as O9.5 V + B1.5 V. A reanalysis of the data with V662 Car = FO 15 = ALS 16081. We have MGB has allowed us to classify it as an SB2 with O9.2 IV + B1: V, similar to the Sana et al. reanalyzed the data for this SB2 to change the v classification of O5 Vz + B0: V of paper II to (2008) result. The system was caught at a ∆ of ∼ O5 V(n)z + B0: V:. The system was caught at a 450 km/s. ∆v of ∼625 km/s. HD 156292 = ALS 4055. In paper II we did not detect the SB2 nature of this target in the HDE 305525. In paper II we classified this GOSSS spectra, even though it is a system of that object as O5.5 V(n)((f))z, that is, with broad nature as revealed by OWN (Barb´aet al. 2010). lines but without identifying it as a spectroscopic A reanalysis of the data with MGB has allowed binary. A reanalysis of the data allowed us to us to derive an O9.7 III + B spectral classification discover that [a] the broad lines were caused with a ∆v of ∼350 km/s. by another O star blueshifted by ∼175 km/s and [b] the He i lines (but not the He ii ones) had a third absorption component redshifted by HDE 319703 A = ALS 4081 A. In paper II ∼400 km/s, indicating the presence of a B star we did not detect the SB2 nature of this target as an additional spectroscopic component. There- in the GOSSS spectra, even though it is a system fore, we classify this is a new SB3 system (the of that nature as revealed by OWN (Barb´aet al. first one identified as such with GOSSS) with 2010). A reanalysis of the data with MGB has al- spectral types O5.5 V((f))z + O7.5 V + B. A lowed us to derive an O7 V((f)) + O9.5 V spectral revision of OWN data confirms the SB3 na- classification with a ∆v of ∼175 km/s. ture, as it appears that way in at least one epoch. We looked at the ASAS All-Star Catalogue HD 158186 = V1081 Sco = ALS 4182. In (http://www.astrouw.edu.pl/asas/?page=aasc) paper II we did not detect double lines in this tar- and we identified HDE 305 525 as an eclipsing bi- get in the GOSSS spectra, even though it is an SB3 nary with a 1.9018 d period. system as revealed by OWN (Barb´aet al. 2010). A reanalysis of the data with MGB has allowed us δ Cir AaAbAc = HD 135 240 AaAbAc to derive an SB2 O9.2 V + B1: V spectral classi- = ALS 3331 AaAbAc. In paper II we did fication with a ∆v of ∼375 km/s. not detect double lines in this object in the 3.2. New systems in GOSSS GOSSS spectra, even though it is an SB3 system (Penny et al. 2001), who classified it as O7 III- In Table 5 we list the new O-type stellar sys- V + O9.5 V + B0.5 V. A reanalysis of the data tems incorporated into GOSSS in this paper, or- with MGB has allowed us to classify it as an SB2 dered by GOSSS ID. The corresponding spectro- with O7 IV((f)) + B, which is consistent with the grams are shown in the same order in Fig. 2. We Penny et al. (2001) result considering that we see present here additional information about each only two components and they detect three. The one of the systems. system was caught at a ∆v of ∼300 km/s. In the component nomenclature AaAb corresponds ALS 19618 = NGC 6618 Sch-1. Crampton et al. to the inner, short period 3.9 d binary (though (1978) classified this NGC 6618 star as O5 V. We the system remains unresolved at the time of the obtain an earlier spectral type of O4 V(n)((fc)).

13 ftejunlfraclrvrino hsfigure.] this of sort version are color targets a The for stars. journal GOSSS the new of for Spectrograms 2.— Fig. 0.0 0.5 1.0 1.5 2.0 2.5 3.0 3.5 4.0 4.5

ε 0045 504750 4500 4250 4000 H

He I 4009 He I+II 4026

N IV 4058 C III 4068 / 69 / 70 Si IV 4089 Hδ N III 4097 Si IV 4116 He I 4121 BD ALS 19618O4V(n)((fc)) BD ALS 4626ON6V((f)) ALS 4923O8.5V+ BD V479 SctON6V((f))z HD 168137AaAbO8Vz He I 4144 − − − 16 4826O5.5V((f))z 14 5014O7.5V(n)((f)) 14 5040O5.5V(n)((f)) He I 4169 DIB is 4179 C III 4187 He II 4200

DIB is 4273

Hγ Wavelength (Å) N III 4379 He I 4388 14 DIB is 4428 He I 4438

He I 4471

DIB is 4502 N III 4511 / 15

He II 4542 db O D Seteeetoi version electronic the [See ID. GOS by ed Si III 4553 Si III 4568 / 75 DIB is 4591 N V 4604 / 20 Si IV 4631 N III 4634 / 41 / 42 Si IV 4654 C III 4647 / 50 / 51

He II 4686

He I 4713 DIB is 4727

DIB is 4762 / 65 / 80

Si III 4813 / 20 / 29

Hβ DIB is 4880 / 87 N III 4905 He I 4922 i.2—(continued). 2.— Fig. 0.0 0.5 1.0 1.5 2.0 2.5 3.0 3.5 4.0 4.5

ε 0045 504750 4500 4250 4000 H

He I 4009 He I+II 4026

N IV 4058 C III 4068 / 69 / 70 Si IV 4089 Hδ N III 4097 Si IV 4116 He I 4121 BD HD 168461O7.5V((f))Nstr ALS 4880O6V((f)) HD 168504O7.5V(n)z ALS 15360O7V((f))z BD ALS 18929O9.7 HD 175514O7V(n)((f))z+B He I 4144 − − 10 4682O7Vn((f)) 04 4503O7V He I 4169 DIB is 4179 C III 4187 He II 4200

DIB is 4273

Hγ Wavelength (Å) N III 4379 He I 4388 15 DIB is 4428 He I 4438

He I 4471

DIB is 4502 N III 4511 / 15

He II 4542 Si III 4553 Si III 4568 / 75 DIB is 4591 N V 4604 / 20 Si IV 4631 N III 4634 / 41 / 42 Si IV 4654 C III 4647 / 50 / 51

He II 4686

He I 4713 DIB is 4727

DIB is 4762 / 65 / 80

Si III 4813 / 20 / 29

Hβ DIB is 4880 / 87 N III 4905 He I 4922 i.2—(continued). 2.— Fig. 0.0 0.5 1.0 1.5 2.0 2.5 3.0 3.5 4.0 4.5

ε 0045 504750 4500 4250 4000 H

He I 4009 He I+II 4026

N IV 4058 C III 4068 / 69 / 70 Si IV 4089 Hδ N III 4097 Si IV 4116 He I 4121 HDE 228779O9Iab HDE 227245O7V((f))z HDE 227018O6.5V((f))z HDE 227465O7V((f)) HDE 338916O7.5Vz HDE 338931O6III(f) HDE 344758O8.5V(n)((f)) HDE 344777O7.5Vz He I 4144

He I 4169 DIB is 4179 C III 4187 He II 4200

DIB is 4273

Hγ Wavelength (Å) N III 4379 He I 4388 16 DIB is 4428 He I 4438

He I 4471

DIB is 4502 N III 4511 / 15

He II 4542 Si III 4553 Si III 4568 / 75 DIB is 4591 N V 4604 / 20 Si IV 4631 N III 4634 / 41 / 42 Si IV 4654 C III 4647 / 50 / 51

He II 4686

He I 4713 DIB is 4727

DIB is 4762 / 65 / 80

Si III 4813 / 20 / 29

Hβ DIB is 4880 / 87 N III 4905 He I 4922 i.2—(continued). 2.— Fig. 0.0 0.5 1.0 1.5 2.0 2.5 3.0 3.5 4.0 4.5

ε 0045 504750 4500 4250 4000 H

He I 4009 He I+II 4026

N IV 4058 C III 4068 / 69 / 70 Si IV 4089 Hδ N III 4097 Si IV 4116 He I 4121 HD 194649ABO6.5V((f)) ALS 11355O8V(n)((f)) HDE 229202O7.5V(n)((f)) BD +364145O8.5V(n) HD 193595O7V((f)) HD 193682O4.5IV(f) ALS 18707O6.5V((f))z HDE 228854O6IVnvar+O5Vn He I 4144

He I 4169 DIB is 4179 C III 4187 He II 4200

DIB is 4273

Hγ Wavelength (Å) N III 4379 He I 4388 17 DIB is 4428 He I 4438

He I 4471

DIB is 4502 N III 4511 / 15

He II 4542 Si III 4553 Si III 4568 / 75 DIB is 4591 N V 4604 / 20 Si IV 4631 N III 4634 / 41 / 42 Si IV 4654 C III 4647 / 50 / 51

He II 4686

He I 4713 DIB is 4727

DIB is 4762 / 65 / 80

Si III 4813 / 20 / 29

Hβ DIB is 4880 / 87 N III 4905 He I 4922 i.2—(continued). 2.— Fig. 0.0 0.5 1.0 1.5 2.0 2.5 3.0 3.5 4.0 4.5

ε 0045 504750 4500 4250 4000 H

He I 4009 He I+II 4026

N IV 4058 C III 4068 / 69 / 70 Si IV 4089 Hδ N III 4097 Si IV 4116 He I 4121 Cyg OB2 2MASS J20315961+4114504O7.5Vz Cyg OB2 Cyg OB2 BD +404179O8Vz LS III+4114O9.5V(n) HDE 228759O6.5V(n)((f))z He I 4144

He I 4169 − − DIB is 4179 − A11 O7Ib(f) A24 O6.5III(f) B17 O6Iaf+O9:Ia: C III 4187 He II 4200

DIB is 4273

Hγ Wavelength (Å) N III 4379 He I 4388 18 DIB is 4428 He I 4438

He I 4471

DIB is 4502 N III 4511 / 15

He II 4542 Si III 4553 Si III 4568 / 75 DIB is 4591 N V 4604 / 20 Si IV 4631 N III 4634 / 41 / 42 Si IV 4654 C III 4647 / 50 / 51

He II 4686

He I 4713 DIB is 4727

DIB is 4762 / 65 / 80

Si III 4813 / 20 / 29

Hβ DIB is 4880 / 87 N III 4905 He I 4922 i.2—(continued). 2.— Fig. 0.0 0.5 1.0 1.5 2.0 2.5 3.0 3.5 4.0 4.5

ε 0045 504750 4500 4250 4000 H

He I 4009 He I+II 4026

N IV 4058 C III 4068 / 69 / 70 Si IV 4089 Hδ N III 4097 Si IV 4116 He I 4121 Cyg OB2 Cyg OB2 ALS 15119O9.5IV(n) ALS 15144O9.7III(n) Cyg OB2 ALS 15134O8Vz Cyg OB2 ALS 15108ABO6IV((f)) He I 4144

He I 4169 − − − DIB is 4179 − 16 O7.5IV(n) 17 O8V 22 DO9.5Vn 5 BO6.5Iabfp C III 4187 He II 4200

DIB is 4273

Hγ Wavelength (Å) N III 4379 He I 4388 19 DIB is 4428 He I 4438

He I 4471

DIB is 4502 N III 4511 / 15

He II 4542 Si III 4553 Si III 4568 / 75 DIB is 4591 N V 4604 / 20 Si IV 4631 N III 4634 / 41 / 42 Si IV 4654 C III 4647 / 50 / 51

He II 4686

He I 4713 DIB is 4727

DIB is 4762 / 65 / 80

Si III 4813 / 20 / 29

Hβ DIB is 4880 / 87 N III 4905 He I 4922 i.2—(continued). 2.— Fig. 0.0 0.5 1.0 1.5 2.0 2.5 3.0 3.5 4.0 4.5

ε 0045 504750 4500 4250 4000 H

He I 4009 He I+II 4026

N IV 4058 C III 4068 / 69 / 70 Si IV 4089 Hδ N III 4097 Si IV 4116 He I 4121 ALS 15125O9.5IV: Cyg OB2 Cyg OB2 Cyg OB2 Cyg OB2 ALS 15111O8V ALS 15115O8V Cyg OB2 He I 4144

He I 4169 − − − − DIB is 4179 − 10 O9.7Iab 25 AO8Vz 73 O8Vz+ 27 ABO9.7V(n)+V:(n) 6 O8.5V(n) C III 4187 He II 4200

DIB is 4273

Hγ Wavelength (Å) N III 4379 He I 4388 20 DIB is 4428 He I 4438

He I 4471

DIB is 4502 N III 4511 / 15

He II 4542 Si III 4553 Si III 4568 / 75 DIB is 4591 N V 4604 / 20 Si IV 4631 N III 4634 / 41 / 42 Si IV 4654 C III 4647 / 50 / 51

He II 4686

He I 4713 DIB is 4727

DIB is 4762 / 65 / 80

Si III 4813 / 20 / 29

Hβ DIB is 4880 / 87 N III 4905 He I 4922 i.2—(continued). 2.— Fig. 0.0 0.5 1.0 1.5 2.0 2.5 3.0 3.5 4.0 4.5

ε 0045 504750 4500 4250 4000 H

He I 4009 He I+II 4026

N IV 4058 C III 4068 / 69 / 70 Si IV 4089 Hδ N III 4097 Si IV 4116 He I 4121 LS III+4611O3.5If*+ LS III+4612O4.5IV(f) Bajamar StarO3.5III(f*)+O8: BD +453216AO5V((f))z BD +433654O4If Cyg OB2 ALS 15114O7.5V(n)((f)) He I 4144

He I 4169

DIB is 4179 −

29 O7.5V(n)((f))z C III 4187 He II 4200

DIB is 4273

Hγ Wavelength (Å) N III 4379 He I 4388 21 DIB is 4428 He I 4438

He I 4471

DIB is 4502 N III 4511 / 15

He II 4542 Si III 4553 Si III 4568 / 75 DIB is 4591 N V 4604 / 20 Si IV 4631 N III 4634 / 41 / 42 Si IV 4654 C III 4647 / 50 / 51

He II 4686

He I 4713 DIB is 4727

DIB is 4762 / 65 / 80

Si III 4813 / 20 / 29

Hβ DIB is 4880 / 87 N III 4905 He I 4922 i.2—(continued). 2.— Fig. 0.0 0.5 1.0 1.5 2.0 2.5 3.0 3.5 4.0 4.5

ε 0045 504750 4500 4250 4000 H

He I 4009 He I+II 4026

N IV 4058 C III 4068 / 69 / 70 Si IV 4089 Hδ N III 4097 Si IV 4116 He I 4121 ALS 12619O7V((f))z ALS 12370O6.5Vnn((f)) ALS 12320O7IV((f)) BD +552722BO9.5V BD +552722CO7V(n)z+B BD +552722AO8Vz ALS 12050O5V((f)) ALS 11761O9.2II He I 4144

He I 4169 DIB is 4179 C III 4187 He II 4200

DIB is 4273

Hγ Wavelength (Å) N III 4379 He I 4388 22 DIB is 4428 He I 4438

He I 4471

DIB is 4502 N III 4511 / 15

He II 4542 Si III 4553 Si III 4568 / 75 DIB is 4591 N V 4604 / 20 Si IV 4631 N III 4634 / 41 / 42 Si IV 4654 C III 4647 / 50 / 51

He II 4686

He I 4713 DIB is 4727

DIB is 4762 / 65 / 80

Si III 4813 / 20 / 29

Hβ DIB is 4880 / 87 N III 4905 He I 4922 i.2—(continued). 2.— Fig. 0.0 0.5 1.0 1.5 2.0 2.5 3.0 3.5 4.0 4.5

ε 0045 504750 4500 4250 4000 H

He I 4009 He I+II 4026

N IV 4058 C III 4068 / 69 / 70 Si IV 4089 Hδ N III 4097 Si IV 4116 He I 4121 BD +602635O6V((f)) Sh 2 Sh 2 ALS 12749O9V HD 213023AO7.5Vz BD +622078O7V((f))z ALS 12688O5.5V(n)((fc))+B BD +552840O7.5V(n) He I 4144 − − 158 1O3.5V((f*))+O9.5:V 158 2O9.5:V+B0.5: He I 4169 DIB is 4179 C III 4187 He II 4200

DIB is 4273

Hγ Wavelength (Å) N III 4379 He I 4388 23 DIB is 4428 He I 4438

He I 4471

DIB is 4502 N III 4511 / 15

He II 4542 Si III 4553 Si III 4568 / 75 DIB is 4591 N V 4604 / 20 Si IV 4631 N III 4634 / 41 / 42 Si IV 4654 C III 4647 / 50 / 51

He II 4686

He I 4713 DIB is 4727

DIB is 4762 / 65 / 80

Si III 4813 / 20 / 29

Hβ DIB is 4880 / 87 N III 4905 He I 4922 BD -16 4826 = ALS 4944. Hiltner & Johnson (1969). Sana et al. (2009) found it to be a long- (1956) classified this NGC 6618 star as O5 and period SB2 with spectral types O7 V + O8 V and Garmany & Vacca (1991) as O3 V. Our GOSSS Sana et al. (2014) was able to marginally resolve data yield O5.5 V((f))z. Some lines are asymmet- the two components. The SB2 character is not ric, indicating the possiblity of the system being visible in the GOSSS data and we derive a classi- an SB2. Williams et al. (2013) classify this system fication of O8 Vz. as an SB1 and give a period of 15.8 d but note that their observations span less than a full orbit. ALS 15360 = NGC 6611-222. This NGC 6611 star was classified as O7 III((f)) by Hillenbrand et al. ALS 4923. Vijapurkar & Drilling (1993) classi- (1993). Using GOSSS data we obtain O7 V((f))z. fied this star as a rapid-rotator giant, O9.5 IIInn. GOSSS data reveal that it is really an SB2 com- HD 168504 = ALS 4935. This star was posed of two nearly identical main-sequence stars, classified as O8 by Morgan et al. (1955) and as with spectral types of O8.5 V + O8.5 V. The sys- O8 III((f)) by Conti (1973). We derive a classifi- v ∼ tem was caught with a ∆ of 400 km/s, so it is cation of O7.5 V(n)z from GOSSS data. likely to have a short period.

ALS 4880. Vijapurkar & Drilling (1993) clas- ALS 4626. Drilling & Perry (1981) classified sify this star as O5 V. We obtain a classification this star as O5 V. We obtain a classification of of O6 V((f)) with GOSSS data and we select it as ON6 V((f)). a new standard star for this type.

BD -14 5014 = ALS 4981. Crampton et al. HD 168461 = ALS 4931. Hiltner & Johnson (1978) classified this star as O8: V: and Vijapurkar & Drilling (1956) give a classification of O8 for this object. (1993) as O9.5 V. We obtain O7.5 V(n)((f)). The Our result using GOSSS data is O7.5 V((f)) Nstr. star has a visual companion listed in the WDS (2MASS J18222221-1437151) with a last known separation in 2007 of 7′′. 2. We obtained a separate BD -10 4682 = ALS 9584. Hiltner & Johnson spectrum of the companion and we found that it (1956) classify this star as O7 and Garmany & Vacca is a K star, so the proximity is likely to be the (1991) as O7 V. We classify it as O7 Vn((f)) with product of a chance alignment, which agrees with GOSSS data. the difference in proper motions between the two objects. BD -04 4503 = ALS 9772. Hiltner & Johnson (1956) classify this star as O7. We obtain O7 V V479 Sct = ALS 5039. This γ-ray binary using GOSSS data. (Aharonian et al. 2005) was classified as O7 V((f)) by Motch et al. (1997) and as O6.5 V((f)) by HD 175514 = V1182 Aql = BD +09 3928 Clark et al. (2001). We derive a slightly earlier = ALS 10048. Hiltner & Johnson (1956) orig- classification of ON6 V((f))z from GOSSS data. inally classified this star as O8 Vnn. The star was later discovered to be an eclipsing SB2 and BD -14 5040 = ALS 5025 = LS IV -14 57. Bell et al. (1987) obtained a spectral classification We classify this star as O5.5 V(n)((f)) which, to of O9 Vnn + B3 V. We also see it as an SB2 our knowledge, is the first spectroscopic identifi- with GOSSS but the new spectral classification, cation of this target as an O star. Note that the O7 V(n)((f))z + B implies a significantly earlier characterization of the object by Kilkenny (1993) primary. The system was caught with a ∆v of was based purely on photometry. ∼ 425 km/s.

HD 168 137 AaAb = ALS 4915 AaAb = ALS 18929 = LSE 107. This star appears NGC 6611-401 AaAb. This NGC 6611 sys- as Osp... in Simbad but there are no references tem was classified as O8 V by Hiltner & Morgan

24 listed for that classification. Indeed, the only ref- HDE 338916 = BD +25 3952 = ALS 10493. erences for this star that appear in the ADS are Hiltner & Johnson (1956) classified this star as Reed (2003, 2005) but there is no spectral type O8. The GOSSS spectral classification is O7.5 Vz. there either. One possibility is that the Simbad classification is a photometric one, not a real spec- HDE 227465 = BD +33 3717 = ALS 10789. 3 tral classification . Another possiblity is that the Hiltner & Johnson (1956) classified this star as Simbad classification comes from the OB- classi- O7:. The GOSSS spectral classification is O7 V((f)). fication in Drilling & Bergeron (1995). Since this object is an O9.7 in the GOSSS data, this is the first time it receives an O-type spectral classifica- HDE 227018 = BD +34 3828 = ALS 10695. tion. The star has sharp lines, indicating a low Hiltner & Johnson (1956) classified this star as v sin i but we are unable to give a luminosity class O7. The GOSSS spectral classification is O6.5 V((f))z. because it is a good example of the problem dis- cussed in Appendix A.2 of Walborn et al. (2014). HDE 227245 = BD +35 3924 = ALS 10 744. For late-O stars there are two luminosity crite- Hiltner & Johnson (1956) classified this star as ria, the ratios of He ii λ4686 to He ii λ4713 and of O7. The GOSSS spectral classification is O7 V((f))z. Si iv λ4089 to He i λ4026, respectively (Table 6 in paper I). For the majority of O9.5-O9.7 stars the HDE 228779 = BD +34 3961 = ALS 11098. two criteria agree but in some cases they yield dif- Hiltner & Johnson (1956) classified this star as ferent answers, with the second criterion providing O9.5 Ib. The GOSSS spectral classification is results that are more consistent with the distance O9 Iab. to 30 Doradus for the O9.5-O9.7 stars analyzed there. In the case of ALS 18929, the first criterion yields a luminosity class of II while the second one HDE 228854 = V382 Cyg = BD +35 4062 yields a luminosity class of V. Given the discrep- = ALS 11132. Pearce (1952) assigned spectral ancy, we do not assign a luminosity class to this types of O6.5 and O7.5 to the two components of object. When observing ALS 18929, we placed a this overcontact eclipsing binary with a period of nearby star, Tyc 1036-00534-1, on the slit and it just 1.8855 d. The GOSSS spectral classification turned out to have an F spectral type. is O6 IVn var + O5 Vn var, with the O6 listed first because it is the brighter component. The system was caught at a ∆v of ∼ 575 km/s. The var suffix HDE 344777 = ALS 10425. Turner (1979) is used because we have another GOSSS observa- classified this star as O9.5 III:. We agree that it tion near conjunction with a spectral type that is is an O star but the GOSSS spectral classification incompatible with the two observed near quadra- is rather different, O7.5 Vz. ture: the combined spectral subtype is O7 and there is a clear N iii λ4634-41-42 emission (that is HDE 344758 = BD +24 3843 = ALS 10421. absent in the near quadrature spectrum). Hiltner & Johnson (1956) classified this star as O8 V. The GOSSS spectral classification is ALS 18707 = S104 Anon 3. Crampton et al. O8.5 V(n)((f)). (1978) classified this star as O6 V. The GOSSS spectral classification is O6.5 V((f))z. There is a HDE 338931 = BD +24 3881 = ALS 10512. companion ∼3 magnitudes fainter towards the SW Hiltner & Johnson (1956) classified this star as at a distance of 2′′. 1 that we were able to spatially O6f. The GOSSS spectral classification is O6 III(f) resolve in our long-slit spectra: it is an early B and we select it as the new standard star for this star. The two objects appear to be the brightest type. stars in an obscured clusetr.

3We discuss below other cases where the lack of references for Simbad classifications do not allow for their verification. HD 193682 = ALS 11181. Hiltner & Johnson (1956) classified this star as O5. Using GOSSS data we obtain O4.5 IV(f). It is one of the new

25 O4-O5.5 IV stars and we use it as one of the new Cyg OB2-B17 = V1827 Cyg = [CPR2002] B17. standards. Stroud et al. (2010) discovereed that this is an SB2 system composed of two O supergiants with HD 193595 = ALS 11162. Roman (1951) spectral types O7 Iaf and O9 Iaf and a period of classified this star as O8 and Morgan et al. (1953) 4.0217 d. We obtained one GOSSS epoch in which as O7. The GOSSS spectral classification is the two components are clearly separated, as the ∼ O7 V((f)). system was caught with a ∆v of 450 km/s, and we obtained a spectral type of O6 Iaf + O9: Iaf. The spectral type of the primary is earlier that the BD +36 4145 = ALS 11453. Hiltner & Johnson Stroud et al. (2010) result, possibly because of our (1956) classified this star as O9 V and Negueruela et al. better spectral resolution. The uncertainty in the (2004) as O8.5 V. The GOSSS spectral classifica- secondary spectral type arises from inconsistencies tion is O8.5 V(n). among some He ii lines, possibly caused by the strong winds evidenced by the observed emission HDE 229202 = BD +39 4162 = ALS 11274. lines. Indeed, He ii λ4686 and N iii λ4634-41-42 Hiltner & Johnson (1956) classified this star as for the primary appear as strong in emission for O8: V. The GOSSS spectral classification is the primary as for some O Iafpe stars but we can- O7.5 V(n)((f)). not give it that designation because He i λ4471 does not show a P-Cygni profile. In any case, ALS 11355 = LS II +39 53. Vijapurkar & Drilling this system clearly deserves follow-up with a high- (1993) classified this star as O7 V:. The GOSSS resolution spectrograph on a 10 m-class telescope. spectral classification is O8 V(n)((f)). When observing this target, we placed a nearby star, Cyg OB2-A24 = 2MASS J20344410+4051584 2MASS J20272914+3945054, on the slit and it = [CPR2002] A24. Negueruela et al. (2008) turned out to have a G spectral type. classified this star as O6.5 III((f)). The GOSSS spectral classification is O6.5 III(f), see Table 2 in paper II. The star Cyg OB2-A27 is located HD 194649 AB = ALS 11324. Hiltner & Johnson ′′ (1956) classified this star as O6.5. The GOSSS 13. 8 away and was placed on the slit. We obtain spectral classification is O6.5 V((f)). The WDS a spectral classification of B0 Ia, consistent with lists a companion 0′′. 4 to the SW with a ∆m of the Hanson (2003) result. 0.6 that we are unable to separate in the GOSSS spectra but that is easily seen in unpublished As- 2MASS J20315961+4114504. Comer´on & Pasquali traLux lucky images (Ma´ızApell´aniz 2010). (2012) classified this star as O7 V. The GOSSS spectral classification is O7.5 Vz. WR 144 is lo- ′′ HDE 228759 = BD +41 3689 = ALS 11083 cated 48. 7 away from this star and was placed on = LS III +41 15. Mayer & Mac´ak (1971) clas- the slit. sified this star as O6. The GOSSS spectral classifi- cation is O6.5 V(n)((f))z. LS III +41 14 is located Cyg OB2-A11 = ALS 21079 = [MT91] 267 30′′ away and was observed simultaneously. = [CPR2002] A11. Negueruela et al. (2008) classified this target as O7 Ib-II(f) and Kobulnicky et al. LS III +41 14 = ALS 11081. Mayer & Mac´ak (2012) identified it as an SB1 system with a (1971) classified this star as O9 V. The GOSSS 15.511 d period. The GOSSS spectral classifi- cation is very similar, O7 Ib(f). Cyg OB2-A11 is spectral classification is O9.5 V(n). HDE 228 759 ′ is located 30′′ away and was observed simultane- 1.8 away from Cyg OB2-12, a well known, highly ously. extinguished B hyper/supergiant (Morgan et al. 1954; Walborn et al. 2015) which we placed on the slit and for which we found a spectral type of BD +40 4179 = ALS 11363. Hiltner & Johnson B5 Ia. Note, however, that this star is a photomet- (1956) classified this star as O8: V. The GOSSS ric variable (Salas et al. 2015) and that for late B spectral classification is O8 Vz.

26 stars the He i λ4471/Mg ii λ4481 ratio is luminos- to our knowledge, it has never been classified as ity dependent, which leads to differing spectral an O star before. subtypes in the literature (Clark et al. 2012). ALS 15119 = [MT91] 588. Massey & Thompson ALS 15108 AB = [MT91] 516 AB. Massey & Thompson(1991) classified this star as B0 V. However, ac- (1991) classified this star as O5.5 V((f)). The cording to GOSSS data it is an O9.5 IV(n) and, GOSSS spectral classification is O6 IV((f)) and to our knowledge, it has never been classified as was obtained with GTC data. Mason et al. (2009) an O star before. We also placed the nearby found a B component with ∆m of 0.4 magnitudes Cyg OB2-18 on the slit: it is an early-B super- 0′′. 7 away (see also Caballero-Nieves et al. 2014). giant, in agreement with previous classifications We were unable to spatially resolve the secondary (e.g. Kiminki et al. 2007). with GOSSS but it is clearly seen in unpublished AstraLux lucky images (Ma´ızApell´aniz 2010). Cyg OB2-17 = ALS 15105 = Schulte 17 = [MT91] 339. Massey & Thompson (1991) Cyg OB2-5 B = V279 Cyg B = BD +40 4220 B classified this star as O8.5 V and according to = Schulte 5 B = ALS 11408 B. Cyg OB2- Kobulnicky et al. (2014) it is an SB1. The GOSSS 5 B is 3 magnitudes dimmer than Cyg OB2-5 A spectral classification is O8 V. This star was ob- and is located 0′′. 934 away (Ma´ızApell´aniz 2010). served placing ALS 15 111 on the same slit. In paper I we mentioned that it is a mid-O star but we were unable to give a precise classification Cyg OB2-16 = LS III +41 33 = ALS 11415 due to the low S/N of the spectrum (the low S/N = Schulte 16 = [MT91] 299. = Cyg OB2- was caused by the contamination from A). We A43 = [CPR2002] A43 Hiltner & Johnson observed the AB pair again with GOSSS and this (1956) classified this star as O8 V. The GOSSS time we were able to clearly separate the two stars, spectral classification is O7.5 IV(n). This star was with the B component being an O6.5 Iabfp. The observed placing Cyg OB2-6 on the same slit. p suffix is used due to the anomalous He ii λ4686 profile. Cyg OB2-6 = LS III +41 35 = ALS 11418 = Schulte 6 = [MT91] 317 = BD +40 4221. ALS 15134 = [MT91] 534. 558] Massey & Thompson Johnson & Morgan (1954) classified this star as (1991) classified this star as O7.5 V. The GOSSS O8 (V). The GOSSS spectral classification is spectral classification is O8 Vz. We also placed on ′ O8.5 V(n). This star was observed placing the slit [MT91] 558, located 1.0 away, and found Cyg OB2-16 on the same slit. it is an F star.

ALS 15115 = [MT91] 485. Massey & Thompson Cyg OB2-22 D = Schulte 51 = [MT91] 425 (1991) classified this star as O8 V and we ob- = ALS 15149. Cyg OB2-22 D is part of the tain the same spectral classification with GOSSS. Cyg OB2-22 Trapezium-like system (Ma´ızApell´aniz Kobulnicky et al. (2014) find it is an eccentric SB1 2010), in which we classified three O stars with a period of 4066 d. in paper I: A, Ba, and C (= V2185 Cyg). Massey & Thompson (1991) classified the D com- ponent as B0 V and several subsequent works ALS 15111 = [MT91] 376. Massey & Thompson repeat this classification. In the GOSSS data, we (1991) classified this star as O8 V and we obtain classify it as O9.5 Vn, which is the first time it the same spectral classification with GOSSS. This has been recognized as an O star. star was observed placing Cyg OB2-17 on the same slit. ALS 15144 = [MT91] 378. Massey & Thompson (1991) classified this star as B0 V and according Cyg OB2-27 AB = ALS 15118 AB = to Kobulnicky et al. (2014) it is an SB1. However, Schulte 27 AB = [MT91] 696 AB. Kiminki et al. according to GOSSS data it is an O9.7 III(n) and, (2015) classified this eclipsing SB2 as O9.5 V + B0.5 V

27 and measured a distance of 1.32 ± 0.07 kpc. and the Si iv λ4089 to He i λ4026 ratios. This star With GOSSS we caught this system with a was observed placing Cyg OB2-29 on the same slit. ∆v of ∼450 km/s and obtain a classification of O9.7 V(n) + O9.7 V:(n). Salas et al. (2015) mea- ALS 15114 = [MT91] 771. 775] This system sured the period of this eclipsing binary as 1.46917 is an SB2 with O7 V + O9 V spectral types and a d and Laur et al. (2015) detected a small period period of 2.82105 d according to Kobulnicky et al. change. Caballero-Nieves et al. (2014) found a B (2014). We only obtained one GOSSS epoch and it companion with a ∆m = 0.94 and a separation of ′′ was at an unfavorable phase, so we can only derive 0. 023. We also placed the nearby [MT91] 674 on a combined spectral type of O7.5 V(n)((f)). We the slit and we found it is a K star. placed the neighbor [MT91] 775 and determined it is a K star. Cyg OB2-73 = Schulte 73. Kiminki et al. (2009) classified this star as O8 III + O8 III and Cyg OB2-29 = ALS 15110 = Schulte 29 measured a period of 17.28 d, which were later = [MT91] 745. Massey & Thompson (1991) revised to O8.5 III: + O9 III: and 34.88 d by classified this star as O7 V and Kobulnicky et al. Kobulnicky et al. (2014). With GOSSS we caught (2014) determined it is an SB1 with a 151.2 d ∼ the system at a ∆v of 175 km/s and we obtain a period. The GOSSS spectral classification is classification of O8 Vz + O8 Vz, clearly excluding O7.5 V(n)((f))z. This star was observed placing the prior giant classifications because the z ratio ALS 15 125 on the same slit. is larger than 1.1 for both components.

BD +43 3654 = ALS 11429. Comer´on & Pasquali Cyg OB2-25 A = ALS 15104 A = Schulte 25 A (2007) classified this object as O4 If and pro- = [MT91] 531 A. Massey & Thompson (1991) posed it is a runaway ejected from Cyg OB2. The classified this system as O8.5 V. The GOSSS spec- GOSSS data yield the same spectral classification. tral classification is O8 Vz and we are able to spatially separate the B component, which turns out to be an early-B star. Caballero-Nieves et al. BD +45 3216 A = ALS 11435 A. Hiltner & Johnson (2014) measure a separation between A and B of (1956) classified this target as O8. GOSSS data 1′′. 45 and a visual ∆m of 0.5 magnitudes, which yields a rather different spectral classification of is consistent with the GOSSS data and with what O5 V and there is a good explanation for the dif- ference. The WDS lists a B companion with a we see in unpublished AstraLux lucky images ′′ (Ma´ızApell´aniz 2010). ∆m of 0.3 mag and a separation of 0. 8 which is clearly seen in our unpublished AstraLux lucky images (Ma´ızApell´aniz 2010). We were able to Cyg OB2-10 = BD +41 3804 = Schulte 10 = obtain GOSSS spectra under good seeing con- [MT91] 632 = ALS 11434. Hiltner & Johnson ditions and spatially separate both components. (1956) classified this system as O9.5 Ia. The The O5 V((f))z classification corresponds to the GOSSS spectral classification is O9.7 Iab. Caballero-NievesA et component al. while the B component is an early (2014) detected a B component with a separation ′′ B star, which explains the previous O8 classifica- of 0. 22 and a ∆m of 2.0 which we were unable tion (a reasonable classification for the combined to spatially separate in the GOSSS data but that spectrum). can be seen in unpublished AstraLux lucky images (Ma´ızApell´aniz 2010). Bajamar Star = 2MASS J20555125+4352246. Comer´on & Pasquali (2005) identified this star as ALS 15125 = [MT91] 736. Massey & Thompson the main ionizing source of the North America (1991) classified this star as O9 V. The GOSSS Nebula4 and classified it as O5 V. We observed spectral classification is O9.5 IV:, with the uncer- tainty in the spectral type arising from the dis- 4We adopt the name “Bajamar Star” for the object due to its crepant results for the He ii λ4686 to He ii λ4713 position relative to the North America Nebula, just to the east of the “Florida Peninsula”. “Islas de Bajamar”, mean-

28 this system several times and we noticed that the ALS 12050 = LS III +57 18. Russeil et al. velocity of the He i lines was not the same as that (2007) classified this star as O5 V. The GOSSS of the He ii and that there were significant vari- spectral classification is O5 V((f)). We also placed ations in the relative velocity (∆v ∼ 300 km/s) the nearby star Tyc 3976-00299-1 on the slit and between epochs. Therefore, the system is an SB2 we found it is an A star. composed of a star earlier than the average type obtained by Comer´on & Pasquali (2005) and a BD +55 2722 A = ALS 12292 A = later star. Our best current spectrum is one where LS III +55 36 A. BD +55 2722 is a Trapezium- we caught the system with the GTC with a ∆v like system at the core of the open cluster ∼ of 100 km/s and from which we assign spec- Teutsch 127. The A component is the brightest tral types of O3.5 III((f*)) + O8:. Note that one and was classified by Mayer & Mac´ak (1973) prior to 2015 there were only two known Galactic as O9 V, though it is likely their result included O stars in the northern hemisphere earlier than also the nearby B component, which we spatially O4, Cyg OB2-7 and Cyg OB2-22 A, see paper I. resolve (see below). The GOSSS spectral classifi- Ma´ızApell´aniz et al. (2015b) added two more (see cation is O8 Vz. below) and in this paper we identify the fifth and the sixth cases (the primary here and the primary of Sh 2-158 1). BD +55 2722 C = LS III +55 37 = ALS 12293. BD +55 2722 C is the wide com- ponent in the BD +55 2722 ABC and is lo- LS III +46 12 = ALS 11449. Mayer & Mac´ak cated 10′′ away from the center of the AB pair. (1973) classified this star as O6. In Ma´ızApell´aniz et al. Crampton et al. (1978) classified it as O7 V. The (2015b,a) we used GOSSS and other data to GOSSS spectral classification is O7 V(n)z + B, study it and classify it as O4.5 V((f)). Here, which is the first time that this system has been we change the luminosity classification to IV with identified as an SB2 to our knowledge. The system the introduction of that class for the spectral sub- was caught at a ∆v of ∼500 km/s. types O4-O5.5. The change from IV to V par- tially (but not completely) alleviates the luminos- ity/distance discrepancy within Berkeley 90 dis- BD+55 2722B =ALS 12292 B=LS III+55 36 B. BD +55 2722 B is the closer companion to cussed in Ma´ızApell´aniz et al. (2015b,a). There- ′′ fore, we cannot yet discard that there is a hidden BD +55 2722 A and is located 1. 7 away with binary component in LS III +46 12. a ∆m of 0.3 mag according to the WDS and con- firmed in our unpublished AstraLux lucky images (Ma´ızApell´aniz 2010). Its existence is referrred LS III +46 11 = ALS 11448. Motch et al. to in several of the papers on BD +55 2722 but, (1997) classified this star as O3-5 III(f)e. In to our knowledge, no spectral type has ever been Ma´ızApell´aniz et al. (2015b,a) we used GOSSS published (see e.g. Saurin et al. 2010). We placed and other data to discover it is an eccentric mas- the slit along the AB position angle and we were sive SB2 binary with two similar components, each able to spatially separate the two components. with spectral type O3.5 If*. As previously men- The GOSSS spectral type for BD +55 2722 B is tioned, the spectral classification of this 97.3 d O9.5 V, making it the third O star in the Trapez- binary raised the number of northern-hemisphere ium system. Galactic O stars earlier than O4 to four objects.

ALS 12320 = LS III +55 45. McCuskey ALS 11761 = LS III +46 50. Negueruela & Marco (1955) classified this object as O8. The GOSSS (2003) classified this star as O9.5 III. The GOSSS spectral classification is O7 IV((f)) and we use it spectral classification is O9.2 II and we use it as as one of the new standards. The nearby star one of the new standards. 2MASS J22202471+5608080 was also placed on the slit: it is a late-B star. ing “low-tide islands” in Spanish, was the original name of the Bahamas islands because many of them are only easily seen from a ship during low tide.

29 ALS 12370 = LS III +55 65. Hiltner (1956) this object and Sh 2-158 1 (see below) are classified this object as O5. The GOSSS spectral the two ionizing stars of the H ii region Sh 2- classification is O6.5 Vnn((f)). 158 2 (or NGC 7538) while the bright nearby 2MASS J23133680+6130395 is a K star (which ALS 12619 = LS III +57 90. Massey et al. we confirmed by placing one of our slits on it). (1995) classified this star as O8 V((f)). The However, they only provided rough spectral types GOSSS spectral classification is O7 V((f))z. of O7 for both sources. We have observed Sh 2- 158 2 with GOSSS and found that it is an SB2 caught with a ∆v of ∼ 275 km/s and spectral BD +55 2840 = ALS 12685. Hiltner & Johnson types O9.5: V + B0.5: V. Those are significantly (1956) classified this star as O7.5p. The GOSSS later than O7, so we suspect that the previous spectral classification is O7.5 V(n). classification was intended for Sh 2-158 1 (though that is also inaccurate, see below). ALS 12688 = LS III +56 109. This star ap- pears as O. . . in Simbad but we have not found Sh 2-158 1 = Tyc 4279-01463-1. As for the any reference to any spectral classification, so we previous object, there is little information about suspect the reason for the listing is a photometric Sh 2-158 1 in the literature. That is why we classification. We have found it to be not only an were surprised to find out with GOSSS that it O star but an SB2 as well. The GOSSS spectral is a very early type SB2 caught with the GTC type is O5.5 V(n)((fc)) + B, with the compan- with a ∆v of ∼375 km/s and spectral types of i ion having He λ4471 in absorption but no sign O3.5 V((f*)) + O9.5: V. As previously mentioned, ii of He λ4542 (hence, we can only classify it as a the primary of this system is the fifth Galac- B) and this system being caught on two different tic O star earlier than O4 in the northern hemi- epochs with a ∆v of 500 km/s. Lewandowski et al. sphere (the sixth is the primary of the Bajamar (2009) confirm the binary nature of the system Star, see above). Most of the He i λ4471 absorp- by identifying it as an eclipsing binary with a tion originates in the secondary while most of the 2.02170 d period. He ii λ4542 absorption originates in the primary. If the absorption is considered to originate in a BD +62 2078 = ALS 12408. Hiltner & Johnson single object, the combined spectral type would (1956) classified this star as O7. The GOSSS spec- be O4.5 (which is still too early to explain the tral classification is O7 V((f))z. previous classification as O7).

HD 213023 A = BD +62 2081 = ALS 12424. BD +60 2635 = ALS 13256. Martin (1972) Morgan et al. (1955) classified this star as O9 V:. classified this star as O9 III. The GOSSS spec- The GOSSS spectral classification is O7.5 Vz, tral classification is O6 V((f)). The original clas- which is significantly different. We suspect that sification was done with objective-prism data, the reason is that the original spectral type in- so a possible explanation for the discrepancy is cluded the B component, located at a separation the low quality of the original data. However, of 1′′. 7 with a ∆m of 0.4 according to the WDS. Negueruela & Marco (2003) classified this star as The GOSSS spectra spatially separated the two ON7 III(f), which is also discrepant (we see a N components and we obtained an early B spectral enhancement in the GOSSS data but not signif- type for the companion. icant enough to classify it as ON) so it is also possible that the star is variable. ALS 12749 = LS III +56 119. Massey et al. (1995) classified this star as O9.5 V((f)). The BD +66 1661 = ALS 13323. Hiltner & Johnson GOSSS spectral classification is O9 V. (1956) classified this star as O9 V. The GOSSS spectral classification is O9.2 V. Sh 2-158 2 = 2MASS J23133024+6130103. Deharveng et al. (1979) correctly identified that

30 V747 Cep = BD +66 1673 = ALS 13375 it star with GOSSS and found it is an SB2 with = NGC 7822-3. This object is an eclips- spectral types O8 V + B0: V caught with a ∆v of ing binary with a period of 5.33146 d in the 200 km/s. To our knowledge this is the first iden- open cluster Berkeley 59 that was classified as tification of this object as a spectroscopic binary. O5 Vn((f)) by Majaess et al. (2008). The GOSSS spectral type is O5.5 V(n)((f)). No double lines BD +61 411 A = ALS 7203. Hiltner & Johnson were seen in our data. We placed the nearby (1956) classified this star as O6. The GOSSS 2MASS J00015191+6731474 on the slit and found spectral classification is O6.5 V((f))z. There is it is an early B star. a B component detected as a separate source in 2MASS located 5′′. 672 toward the NE. We were BD +66 1675 = ALS 13379. This object is able to spatially separate it from A and we found the brightest star in the open cluster Berkeley 59 it is an early B star. and was classified as O7 by Hiltner & Johnson (1956). The GOSSS spectral classification is ALS 7833 = LS I +57 138. This is one of the O7.5 Vz. two bright stars in the open cluster Alicante 1. Negueruela & Marco (2003) classified it as O7 V. BD +66 1674 = ALS 13378. This object The GOSSS spectral classification is O8 Vz. is the second brightest star in the open clus- ter Berkeley 59 and was classified as O9.5 V by MY Cam = BD +56 864 = ALS 7836. This Bisiacchi et al. (1982). The GOSSS spectral clas- is the second of the two bright stars in the open sification is O9.7 IV:. The uncertainty in the lumi- cluster Alicante 1. Hiltner & Johnson (1956) clas- nosity class is caused by the discrepancy between sified it as O6nn and Lorenzo et al. (2014) discov- ii ii the He λ4686 to He λ4713 criterion (which ered it is an overcontact binary composed of two O iv i yields III) and the Si λ4089 to He λ4026 cri- stars with a period of 1.1754514 d. In the GOSSS terion (which yields V), another example of the data the two components are separated by a ∆v effect previously mentioned. of ∼500 km/s and we assign them spectral types O5.5 V(n) + O6.5 V(n). Tyc 4026-00424-1 = NGC 7822-29 = ALS 17 957. This object is also located in Berkeley 59 and was BD +50 886 = ALS 7868. This object is the classified as O9 by Walker (1965). The GOSSS main ionizing source of the H ii region Sh 2-206 spectral classification is O7 V((f))z. We also (= NGC 1491) and was classified by Moffat et al. placed a nearby star, ALS 13380, on the slit and (1979) as O5neb. The GOSSS spectral classifica- found is an early B star. tion is O4 V((fc)).

ALS 6351 = LS I +62 139. Hiltner & Johnson BD +52 805 = ALS 7928. This object is the (1956) classified this star as O7. The GOSSS spec- brightest star in the open cluster Waterloo 1 and tral classification is O7 Vz. was classified by Moffat et al. (1979) as O9.5 V. The GOSSS spectral classification is O8 V(n). BD +60 134 = ALS 6405. Popper (1950) classified this star as O7. The GOSSS spectral ALS 8272 = LS V +38 12. This object classification is O5.5 V(n)((f)). was classified by Georgelin et al. (1973) as O9 V. We observed it with GOSSS and found it is an HD 5689 = BD +62 178 = ALS 6425. SB2 with spectral types O7 V((f)) + B0 III-V Hiltner & Johnson (1956) classified this star as caught with a ∆v of 325 km/s. To our knowl- O6. The GOSSS spectral classification is O7 Vn((f)). edge this is the first identification of this object as a spectroscopic binary. We placed the neighbor ALS 6967 = LS I +59 112. Hiltner & Johnson HDE 277 990 on the slit and found it is an F star. (1956) classified this object as O9 V. We observed

31 ALS 8294 = LS V +33 15 = NGC 1893-149. HDE 256725 B = BD +19 1339 B = Walker & Hodge (1968) classified this star as O7. ALS 47. This star is the second brightest ob- The GOSSS spectral classification is O7 V(n)z. ject of the Trapezium system HDE 256725 and was classified as O8 III by Moffat et al. (1979). ALS 19265 = Rubin & Losee 128. This ob- The GOSSS spectral type is O9.5 V. ject was classified as O7 V by Chromey (1979), who was searching for O stars at large Galac- Tyc 0737-01170-1 = NGC 2264 +10 60. tocentric radii near the Galactic anticenter. We Voroshilov et al. (1985) classified this star as O5:. find the spectrum to be quite remarkable and we The GOSSS spectral classification is O7 Vz. We classify it as O4.5 V((c))z, with the ((c)) suffix also placed the nearby ALS 9044 and we found it indicating C iii λ4650 emission without apparent is a late-B supergiant. N iii λ4634-41-42 emission, an effect that we have not seen in any other O star. Another peculiarity ALS 85. This star was classified as O9.5 IV by i ii is the difference between the He and He pro- Moffat et al. (1979). Aldoretta et al. (2015) find files. We should caution that ALS 19 265 could be two dim companions. The GOSSS spectral type is an evolved low-mass star. For example, we also ob- O7.5 V. We have applied a CHORIZOS analysis to served another one of the stars in Chromey (1979), this star similar to the one above for ALS 19 265. ALS 19270, and its GOSSS spectrum looks quite If this target is a ZAMS O star it would be lo- similar to that of ALS 19 265 though it is now cated at a distance of ∼7.5 kpc. The inclusion of known to be a planetary nebula nucleus or PNN the mentioned two dim companions would place it (Aller et al. 2015). To investigate this further we slightly closer but if the star is slightly evolved it downloaded the SDSS data for the target. In the should be slightly farther away. Therefore, this is images it appears as a blue object but no nebu- a good candidate for an O star at large Galacto- losity is seen in the r band, as it would be ex- centric radius, something that could be confirmed pected of a PN (the star could still be a naked once the Gaia distance becomes available. sdO). We have also processed the SDSS photom- etry through CHORIZOS (Ma´ızApell´aniz 2004, 2013b; Ma´ızApell´aniz et al. 2014b) assuming that ALS 207. This object is the main ionizing ii ALS 19265 is a ZAMS O star. Under those cir- source of the H region Sh 2-301 (= RCW 6) cumstances, it would have to be located at a dis- and was classified as O7 by Moffat et al. (1979). tance close to 30 kpc and its extinction would have The GOSSS spectral classification is O6.5 V((f)). a large value of R5495 (between 5 and 6, an indi- cation that some of the extinction takes place in BD -15 1909 = ALS 552. Fitzgerald & Moffat an environment depleted of small dust grains such (1980) classified this star as O8. The GOSSS spec- as an H ii region or a PN). Such a large distance tral classification is O6.5 V((f))z. would be extreme for a Galactic O star (with the likely low metallicity providing a possible explana- ALS 458 = Sh 2-306 4. Moffat et al. (1979) tion for the peculiar spectrum) but the available classified this star as O5. The GOSSS spectral information does not exclude the possibility of the classification is O6.5 V((f))z. object being a lower luminosity, lower mass, closer evolved star. Gaia should be able to provide us with a distance measurement and decide between V441 Pup = 4U 0728-25 = ALS 437. the two options. This X-ray binary was classified as O8/9 Ve by Negueruela et al. (1996). The GOSSS spectral classification is O5: Ve. The reason for the dif- HDE 256725 A = BD +19 1339 A = ference in the classifications is that the GOSSS ALS 46. This star is the brightest object of spectral types do not take into consideration the the Trapezium system HDE 256725 and was clas- infilling of He i λ4471 (i.e. they are strict, not cor- sified as O6 by Moffat et al. (1979). The GOSSS rected, spectral types), which is common among spectral type is O5 V((fc)). Oe stars. This is the earliest spectral type we

32 have assigned to an Oe star in GOSSS (the previ- We placed the nearby star Tyc 8608-00069-1 on ous record holder was HD 39680 = V1382 Ori, an the slit and found it is a mid-B star. O6). HD 89625 = CPD -59 2044 = ALS 1492. CPD -26 2704 = ALS 830. This object in the Cannon & Mayall (1949) classified this star as B0 Haffner 18 open cluster was classified as O7k by (chart 135) and Houk & Swift (1999) as B3/4 V:. Fitzgerald & Moffat (1974). The GOSSS spectral The GOSSS spectral type is ON9.2 IVn and is dis- type is O7 V(n). We placed another cluster star, cussed in more detail in Walborn et al. (2016). To ALS 832, on the slit and found it is an early-B our knowledge this object had never been classi- star. fied as an O star.

V467 Vel = CPD -45 2920 = ALS 1135. 2MASS J10224377-5930182 = [VRV91] 85. This system is an SB2 with O6.5 V + B1 V spec- This object is located in the little-studied open tral types and a period of 2.753 d according to cluster [KPS2012] MWSC 1797 (Kharchenko et al. Fern´andez Laj´us & Niemel¨a(2006). We only ob- 2013) and was classified as B0: V by van Genderen et al. tained one GOSSS epoch and it was at an unfa- (1991). We observed it with GOSSS and we found vorable phase, so we can only derive a combined it is an O8 V(n), which is the first time it has been spectral type of O6.5 V(n)((f)). Given the large identified as an O star. We placed the nearby star magnitude difference, the secondary does not seem Hen 3-406 on the slit and found is an early-type to affect the combined spectral type. We placed Be star. Note that van Genderen et al. (1991) in- the nearby Tyc 8151-01072-1 on the slit and found correctly claimed that Hen 3-406 was an O-type is an early-B star. dwarf.

CPD -49 2322 = ALS 1267. This object in 2MASS J10224096-5930305 = [VRV91] 82. the Pismis 11 open cluster was classified as O8 V This object is also located in [KPS2012] MWSC 1797 by Marco & Negueruela (2009). The GOSSS spec- and it was classified as O V: by van Genderen et al. tral type is O7.5 V((f)). (1991). The GOSSS spectral type is O7 V((f))z.

HD 90273. Hoffleit (1956) classified this object ALS 18551. This star in Collinder 228 appears as O7. The GOSSS spectral type is ON7 V((f)). as O5 in Simbad but this is just a photomet- We placed the nearby star HDE 302 748 on the slit ric classification from Wramdemark (1976), not a and found it is a mid-B star. spectroscopic classification. The GOSSS spectral type is O4.5 V(n)z + O4.5 V(n)z with the system caught with a ∆v of ∼450 km/s. This is the first THA 35-II-42 = WR 21a. Niemel¨aet al. time this system is identified as being an SB2 and (2006) discovered that this star is a binary, as- having an O-type spectral classification. signed it spectral classifications of WN6h + O, and noted that its spectrum resembles that of HD 93 162 (= WR 25). However, as pointed out 2MASS J10584671-6105512. This target in in paper II, Crowther & Walborn (2011) moved Collinder 228 has no current entry in Simbad and, HD 93162 into the early Of/WN (or “early-slash”) to our knowledge, has never been described in any category on the basis of its P-Cygni Hβ profile. publication. We observed it because we placed it Here we do the same with THA 35-II-42 and assign on the same slit as ALS 18553 (see below) and we it a spectral type of O2 If*/WN5. We do not see discovered it is an O8 Iabf, another example of a He i λ4471 from the secondary, which is consistent new O star. with its recent identification by Tramper et al. (2016) as an O3 star, but it is quite possible that ALS 18553. This star in Collinder 228 appears our classification corresponds to a composite spec- as O5+ in Simbad but this just a photometric clas- trum (we only have one epoch with a good S/N). sification from Wramdemark (1976), not a spec- troscopic classification. The GOSS spectral type

33 is O6 IIf, which is the first time this system has NGC 3603 HST-51. Moffat (1983) classi- received an O-type spectral classification. fied this star in NGC 3603 as O4 V(f) and Melena et al. (2008) suggested an earlier type 2MASS J10583238-6110565. This target in with a later companion. The GOSSS spectral Collinder 228 has no current entry in Simbad and, type is O5.5 V(n) but the line profiles are anoma- to our knowledge, has never been described in any lous, indicating that it may indeed be a composite publication. We observed because we placed it on spectrum. the same slit as ALS 18553 (see above) and we discovered it is an O5 V((f)) + O7 V((f)) caught NGC 3603 HST-48. Melena et al. (2008) clas- with a ∆v of ∼200 km/s. This is the first time this sified this star in NGC 3603 as O3.5 If. The system is identified as being an SB2 and having an GOSSS spectral type is the same with the addi- O-type spectral classification. tion of the prescriptive * suffix, i.e. O3.5 If*. We use this object as one of the new standards. THA 35-II-153. This target in Collinder 228 has one single entry in Simbad (The 1966) and no NGC 3603 HST-24. Melena et al. (2008) clas- spectral classification. We observed it because we sified this star in NGC 3603 as O4 V. The GOSSS placed it on the same slit as a repeat observation spectral type is O4 IV(f) and this is one of the new for ALS 2063 (see paper II) and we found it to be O4-O5.5 stars with luminosity class IV. an O3.5 If*/WN7. Early Of/WN stars are quite rare (there are only two in paper II and two more, NGC 3603 MTT 25. Melena et al. (2008) including this one, in this paper) but to find a new classified this star in NGC 3603 as O3 V((f)). The example next to an O Iafpe star such as ALS 2063 GOSSS spectral type is O5 V(n), with He i λ4471 (another rare class with just six examples in paper clearly detected. II) is simply remarkable. What is less surprising is that this coincidence takes place in the Carina Nebula, the richest stellar nursery within 3 kpc of HD 99546 = CPD -58 3620 = ALS 2342. the Sun. Morgan et al. (1955) classified this star as O8. The GOSSS spectral type is O7.5 V((f)) Nstr. HD 97966 = CPD -58 3372 = ALS 2276. Morgan et al. (1955) classified this star as O7.5. HD 110360 = CPD -59 4396 = ALS 2732. The GOSSS spectral classification is O7 V((f))z Morgan et al. (1955) classified this star as O7 and we select it as the new standard star for this and Mathys (1989) identified it as an ON stra. type. Walborn et al. (2011) used GOSSS data to clas- sify it as ON7 Vz. Here, with the new definition of the OVz phenomenon by Arias et al. (2016) we HD 97319 = CPD -60 2606 = ALS 2217. reclassify it as ON7 V. Feast et al. (1961) classified this star as O9.5 Ib. The GOSSS spectral classification is O7.5 IV((f)) and we use it as one of the new standards. We CPD -61 3973 = ALS 3153. Vijapurkar & Drilling placed the nearby HD 97 352 on the slit and found (1993) classified this star as O7 III. The GOSSS it is an early-B star. spectral type is O7.5 V((f)). We placed the slit on the nearby Tyc 9008-01250-1 and found it is an F star. EM Car = HD 97484 = CPD -60 2638 = ALS 2232. Solivella & Niemel¨a(1986) observed this previously known eclipsing SB2 and derived HD 122313 = CPD -61 4286 = ALS 3187. spectral types of O7.5 + O8.5. The GOSSS spec- Houk et al. (1976) classified this star as O5/7. tral types are O7.5 V((f)) + O7.5 V((f)), with the The GOSSS spectral type is O8.5 V. system caught at a ∆v of ∼475 km/s. We placed the nearby object HDE 306190 on the slit and found it is an early-B star.

34 ALS 17591 = [OM80] 35. This object is HDE 328209 AB = CPD -44 7916 = listed as OB+ in Orsatti & Muzzio (1980) but, ALS 3624. Feast et al. (1961) classified this to our knowledge, it has never been classifed as star as O9.5 I(a). The GOSSS spectral type is an O star. With GOSSS we identify it as such ON9 Ib-Iap and is discussed in Walborn et al. and assign it a spectral classification of O5: n(f)p, (2016). OWN data (Barb´aet al. 2010) reveal it noting that He ii λ4686 has a centrally reversed to be a short-period SB2. Unpublished AstraLux (and possibly variable) emission with the red peak Sur images reveal a visual companion (B) about stronger than the blue one. We placed the slit on 3′′ to the East that is unresolved in the GOSSS the nearby Tyc 8706-00582-1 and foud out it is a data. late-B star. HDE 329100 A = ALS 3815. There is some ALS 3386. Bassino et al. (1982) classified this confusion surrounding this double system, starting star as O6 If. The GOSSS spectral type is O6 Iaf. with the current classification of G0 in Simbad, We placed the slit on the nearby Tyc 8696-00095-1 which is clearly wrong. According to the WDS and found it is an F star. there are two components separated by 4′′. 0 with a position angle of 105 degrees and a ∆m of 2 magni- ALS 18049. Georgelin et al. (1994) derived a tudes. We have unpublished AstraLux Sur iz data photometric classification of O7 V for this star but, that are consistent (within small amounts) with to our knowledge, there are no published spec- that information and the 2MASS PSC also points tral classifications. The GOSSS spectral type is in the same direction. Simbad, however, incor- O9 V, making this another case of a first-time O- rectly refers to the western component as B when type spectral classification. Note that ALS 18049 it is really A (the brightest). Crampton (1971) appears to be the ionizing source of a well de- classified the system as O8.5. We were able to fined H ii region seen in both Hα and WISE separate the A (western) and B (eastern) compo- MIR images. We placed the slit on the nearby nents with GOSSS. HDE 329 100 A is an O star 2MASS J15441197-5356471 and found it is an F with spectral type O8 V(n) while the B component star. is an early-B star.

Muzzio III-9. Muzzio (1974) derived a photo- HDE 326775 = CPD -41 7848 = ALS 3906. metric classification of O5+: for this star but, Vijapurkar & Drilling (1993) classified this star as to our knowledge, there are no published spec- O7 V. The GOSSS spectral type is O6.5 V(n)((f))z. tral classifications. The GOSSS spectral type is We placed the nearby Tyc 7877-01317-1 on the slit O8 Ib, making this another case of a first-time O- and found it is a K star. type spectral classification. We placed the slit on the nearby Muzzio III-10 and found it is a B star ALS 18769 = C1715-387-16 = HM 1-16. but the star is weak so the S/N of the spectrum is To our knowledge, this star in the open cluster poor. Havlen-Moffat 1 has never received a spectral clas- sification. We observed it with GOSSS and de- HD 145217 = CPD -49 8996 = ALS 3499. termined its spectral type to be O6 II(f), adding Feast et al. (1961) classified this star as O8. The another O star to the known Galactic sample. GOSSS spectral type is O8 V. However, some weak Si iii and O ii lines are visible, making it likely that HDE 323110 = ALS 4103. Vijapurkar & Drilling this is a composite spectrum of a slightly earlier (1993) classified this star as B0 IIIne. The GOSSS O star and an early-B star. spectral type is ON9 Ia and is discussed in more detail in Walborn et al. (2016). To our knowledge HD 144647. Feast et al. (1961) classified this this object had never been classified as an O star. star as O8. The GOSSS spectral type is O8.5 V(n). Tyc 7370-00460-1 = 2MASS J17181540- 3400061. Gvaramadze et al. (2011) classified

35 this star as O6.5:. The GOSSS spectral type is hand, we have seen some of them fixed in the last O6 V((f)) + O8 V and we caught the system with two years. a ∆v of ∼500 km/s. To our knowledge, this sys- We show in Fig. 3 the spectrograms of the tem had not been characterized as an SB2 before. eleven egregious false positives reported here. The corresponding spectral types and notes are listed ALS 19693 = [N78] 51. Lortet et al. (1984) in Table 6. A preliminary version of this informa- classified this star as O7: V. The GOSSS spectral tion was given by Ma´ızApell´aniz et al. (2015c). type is O6 Vn((f)). In future papers we will present the spectrograms of additional false positives. Pismis 24-15 = ALS 17700 = [N78] 46. 4. Analysis Massey et al. (2001) classified this star as O8 V. The GOSSS spectral type is O7.5 Vz. In this paper we have added 142 O-type systems to the GOSSS sample, raising the total number to ALS 19692 = [N78] 49. Lortet et al. (1984) 590. Here we analyze some statistics and discuss classified this star as O7: V. The GOSSS spectral the status and future of the project. type is O5.5 IV((f)). • Twenty out of the 142 O-type systems (14%) 3.3. Spectral classification errors are first-time spectral classifications as O. Some of those had prior low-quality pho- One of the findings of GOSSS has been that tometric classifications. As a comparison, the number of classification errors related to a smaller number (18) of new O-type sys- O stars in the literature is quite large. In tems were found in papers I+II but the sig- Ma´ızApell´aniz et al. (2013), we showed that the nificantly larger sample there (448) yields percentage of false positives (stellar systems erro- a lower 4%. The percentage difference be- neously classified as O type) in the GOSSS sam- tween papers is expected, as papers I+II ple observed so far was 24.9%. Since then, the were dominated by the brightest and better number has risen above 30% because, in general, studied O stars, leaving less room for new dim stars have more uncertain classifications than discoveries. Indeed, we expect that future bright ones and as GOSSS progresses we are mov- GOSSS papers will include an even larger ing (on average) into higher magnitude values (see fraction of new O stars. below). The majority of the false positives turn out to • We have also discovered eleven new O-type be B stars, which is expected given the spectro- SB2 systems5, of which six have O com- scopic and photometric similitudes between O and panions (O+O) and five have B companions B stars. However, some of the false positives are (O+B), and a new SB3 system (O+O+B). egregious mistakes, since they turn out to be of We should point out that for most of the A-K type. Those cases are sometimes caused by stars in this paper we have only obtained one identification errors (the spectral type corresponds epoch and that the GOSSS spectral resolu- to a different star) or by photometric classifica- tion only allows for the detection of SB2 sys- tions reported as spectral types. tems with large velocity differences. There- We want to especially warn the reader about fore, we strongly suspect that there are still some of the results given by SIMBAD. The spec- many hidden spectroscopic binaries in this tral classifications there are of highly variable paper’s sample. The new SB2 and SB3 sys- quality. Furthermore, some are “legacy classifi- tems are being followed up (with GOSSS cations”, which have been in SIMBAD before a and in some cases with our high-spectral- reference was required and, as a result, cannot be resolution projects OWN, CAFE-BEANS,´ traced back to a source. SIMBAD classifications are corrected from time to time but some of the 5Twelve if you count the recently published system LS III +461 11, whose SB2 nature was also revealed by egregious false positives mentioned here are still GOSSS (Ma´ız Apell´aniz et al. 2015b). there at the time of this writing. On the other

36 i.2—(continued). 2.— Fig. 0.0 0.5 1.0 1.5 2.0 2.5 3.0 3.5 4.0 4.5

ε 0045 504750 4500 4250 4000 H

He I 4009 He I+II 4026

N IV 4058 C III 4068 / 69 / 70 Si IV 4089 Hδ N III 4097 Si IV 4116 He I 4121 HD 5689O7Vn((f)) BD +60134O5.5V(n)((f)) ALS 6351O7Vz Tyc 4026 BD +661674O9.7IV: BD +661675O7.5Vz V747 CepO5.5V(n)((f)) BD +661661O9.2V He I 4144

He I 4169

DIB is 4179 −

00424 C III 4187 He II 4200 − 1 O7V((f))z

DIB is 4273

Hγ Wavelength (Å) N III 4379 He I 4388 37 DIB is 4428 He I 4438

He I 4471

DIB is 4502 N III 4511 / 15

He II 4542 Si III 4553 Si III 4568 / 75 DIB is 4591 N V 4604 / 20 Si IV 4631 N III 4634 / 41 / 42 Si IV 4654 C III 4647 / 50 / 51

He II 4686

He I 4713 DIB is 4727

DIB is 4762 / 65 / 80

Si III 4813 / 20 / 29

Hβ DIB is 4880 / 87 N III 4905 He I 4922 i.2—(continued). 2.— Fig. 0.0 0.5 1.0 1.5 2.0 2.5 3.0 3.5 4.0 4.5

ε 0045 504750 4500 4250 4000 H

He I 4009 He I+II 4026

N IV 4058 C III 4068 / 69 / 70 Si IV 4089 Hδ N III 4097 Si IV 4116 He I 4121 ALS 8294O7V(n)z ALS 8272O7V((f))+B0III BD +52805O8V(n) BD +50886O4V((fc)) MY CamO5.5V(n)+O6.5 ALS 7833O8Vz BD +61411AO6.5V((f))z ALS 6967O8V+B0: He I 4144

He I 4169 DIB is 4179 C III 4187 He II 4200

DIB is 4273 − V

Hγ Wavelength (Å) N III 4379 He I 4388 38 DIB is 4428 He I 4438

He I 4471

DIB is 4502 N III 4511 / 15

He II 4542 Si III 4553 Si III 4568 / 75 DIB is 4591 N V 4604 / 20 Si IV 4631 N III 4634 / 41 / 42 Si IV 4654 C III 4647 / 50 / 51

He II 4686

He I 4713 DIB is 4727

DIB is 4762 / 65 / 80

Si III 4813 / 20 / 29

Hβ DIB is 4880 / 87 N III 4905 He I 4922 i.2—(continued). 2.— Fig. 0.0 0.5 1.0 1.5 2.0 2.5 3.0 3.5 4.0 4.5

ε 0045 504750 4500 4250 4000 H

He I 4009 He I+II 4026

N IV 4058 C III 4068 / 69 / 70 Si IV 4089 Hδ N III 4097 Si IV 4116 He I 4121 BD ALS 207O6.5V((f)) ALS 85O7.5V ALS 458O6.5V((f))z Tyc 0737 HDE 256725BO9.5V HDE 256725AO5V((fc)) ALS 19265O4.5V((c))z He I 4144 − 15 1909O6.5V((f))z He I 4169

DIB is 4179 −

01170 C III 4187 He II 4200 − 1 O7Vz

DIB is 4273

Hγ Wavelength (Å) N III 4379 He I 4388 39 DIB is 4428 He I 4438

He I 4471

DIB is 4502 N III 4511 / 15

He II 4542 Si III 4553 Si III 4568 / 75 DIB is 4591 N V 4604 / 20 Si IV 4631 N III 4634 / 41 / 42 Si IV 4654 C III 4647 / 50 / 51

He II 4686

He I 4713 DIB is 4727

DIB is 4762 / 65 / 80

Si III 4813 / 20 / 29

Hβ DIB is 4880 / 87 N III 4905 He I 4922 i.2—(continued). 2.— Fig. 0.0 0.5 1.0 1.5 2.0 2.5 3.0 3.5 4.0 4.5

ε 0045 504750 4500 4250 4000 H

He I 4009 He I+II 4026

N IV 4058 C III 4068 / 69 / 70 Si IV 4089 Hδ N III 4097 Si IV 4116 He I 4121 THA 35 HD 90273ON7V((f)) CPD V467 VelO6.5V(n)((f)) HD 89625ON9.2IVn CPD V441 PupO5:Ve He I 4144 − − 49 2322O7.5V((f)) 26 2704O7V(n) He I 4169 −

DIB is 4179 II − C III 4187 42 O2If*/WN5 He II 4200

DIB is 4273

Hγ Wavelength (Å) N III 4379 He I 4388 40 DIB is 4428 He I 4438

He I 4471

DIB is 4502 N III 4511 / 15

He II 4542 Si III 4553 Si III 4568 / 75 DIB is 4591 N V 4604 / 20 Si IV 4631 N III 4634 / 41 / 42 Si IV 4654 C III 4647 / 50 / 51

He II 4686

He I 4713 DIB is 4727

DIB is 4762 / 65 / 80

Si III 4813 / 20 / 29

Hβ DIB is 4880 / 87 N III 4905 He I 4922 i.2—(continued). 2.— Fig. 0.0 0.5 1.0 1.5 2.0 2.5 3.0 3.5 4.0 4.5

ε 0045 504750 4500 4250 4000 H

He I 4009 He I+II 4026

N IV 4058 C III 4068 / 69 / 70 Si IV 4089 Hδ N III 4097 Si IV 4116 He I 4121 THA 35 2MASS J10583238 ALS 18553O6II(f) 2MASS J10584671 ALS 18551O4.5V(n)z+ 2MASS J10224096 2MASS J10224377 He I 4144

He I 4169 −

DIB is 4179 II − C III 4187 153 O3.5If*/WN7 He II 4200 − − − − 6110565 O5V((f))+O7 6105512 O8Iabf 5930305 O7V((f))z 5930182 O8V(n)

DIB is 4273

Hγ Wavelength (Å) N III 4379 He I 4388 41 DIB is 4428 He I 4438

He I 4471

DIB is 4502 N III 4511 / 15

He II 4542 Si III 4553 Si III 4568 / 75 DIB is 4591 N V 4604 / 20 Si IV 4631 N III 4634 / 41 / 42 Si IV 4654 C III 4647 / 50 / 51

He II 4686

He I 4713 DIB is 4727

DIB is 4762 / 65 / 80

Si III 4813 / 20 / 29

Hβ DIB is 4880 / 87 N III 4905 He I 4922 i.2—(continued). 2.— Fig. 0.0 0.5 1.0 1.5 2.0 2.5 3.0 3.5 4.0 4.5

ε 0045 504750 4500 4250 4000 H

He I 4009 He I+II 4026

N IV 4058 C III 4068 / 69 / 70 Si IV 4089 Hδ N III 4097 Si IV 4116 He I 4121 NGC 3603MTT25O5V(n) NGC 3603HST NGC 3603HST NGC 3603HST EM CarO7.5V((f))+ HD 97319O7.5IV((f)) HD 97966O7V((f))z He I 4144

He I 4169 DIB is 4179 C III 4187 He II 4200 − − − 24 O4IV(f) 48 O3.5If* 51 O5.5V(n)

DIB is 4273

Hγ Wavelength (Å) N III 4379 He I 4388 42 DIB is 4428 He I 4438

He I 4471

DIB is 4502 N III 4511 / 15

He II 4542 Si III 4553 Si III 4568 / 75 DIB is 4591 N V 4604 / 20 Si IV 4631 N III 4634 / 41 / 42 Si IV 4654 C III 4647 / 50 / 51

He II 4686

He I 4713 DIB is 4727

DIB is 4762 / 65 / 80

Si III 4813 / 20 / 29

Hβ DIB is 4880 / 87 N III 4905 He I 4922 i.2—(continued). 2.— Fig. 0.0 0.5 1.0 1.5 2.0 2.5 3.0 3.5 4.0 4.5

ε 0045 504750 4500 4250 4000 H

He I 4009 He I+II 4026

N IV 4058 C III 4068 / 69 / 70 Si IV 4089 Hδ N III 4097 Si IV 4116 He I 4121 Muzzio III ALS 18049O9V ALS 3386O6Iaf ALS 17591O5:n(f)p HD 122313O8.5V CPD HD 110360ON7V HD 99546O7.5V((f))Nstr He I 4144 −

61 3973O7.5V((f)) He I 4169 DIB is 4179 −

9 O8Ib(f) C III 4187 He II 4200

DIB is 4273

Hγ Wavelength (Å) N III 4379 He I 4388 43 DIB is 4428 He I 4438

He I 4471

DIB is 4502 N III 4511 / 15

He II 4542 Si III 4553 Si III 4568 / 75 DIB is 4591 N V 4604 / 20 Si IV 4631 N III 4634 / 41 / 42 Si IV 4654 C III 4647 / 50 / 51

He II 4686

He I 4713 DIB is 4727

DIB is 4762 / 65 / 80

Si III 4813 / 20 / 29

Hβ DIB is 4880 / 87 N III 4905 He I 4922 i.2—(continued). 2.— Fig. 0.0 0.5 1.0 1.5 2.0 2.5 3.0 3.5 4.0 4.5

ε 0045 504750 4500 4250 4000 H

He I 4009 He I+II 4026

N IV 4058 C III 4068 / 69 / 70 Si IV 4089 Hδ N III 4097 Si IV 4116 He I 4121 Tyc 7370 HDE 323110ON9Ia ALS 18769O6II(f) HDE 326775O6.5V(n)((f))z HDE 329100AO8V(n) HDE 328209ABON9Ib HD 144647O8.5V(n) HD 145217O8V He I 4144

He I 4169

DIB is 4179 −

00460 C III 4187 He II 4200 − 1 O6V((f))+O8V

DIB is 4273 − Iap

Hγ Wavelength (Å) N III 4379 He I 4388 44 DIB is 4428 He I 4438

He I 4471

DIB is 4502 N III 4511 / 15

He II 4542 Si III 4553 Si III 4568 / 75 DIB is 4591 N V 4604 / 20 Si IV 4631 N III 4634 / 41 / 42 Si IV 4654 C III 4647 / 50 / 51

He II 4686

He I 4713 DIB is 4727

DIB is 4762 / 65 / 80

Si III 4813 / 20 / 29

Hβ DIB is 4880 / 87 N III 4905 He I 4922 i.2—(continued). 2.— Fig. 0.0 0.5 1.0 1.5 2.0 2.5

ε 0045 504750 4500 4250 4000 H

He I 4009 He I+II 4026

N IV 4058 C III 4068 / 69 / 70 Si IV 4089 Hδ N III 4097 Si IV 4116 He I 4121 ALS 19692O5.5IV(f) Pismis 24 ALS 19693O6Vn((f)) He I 4144

He I 4169 DIB is 4179 −

15 O7.5Vz C III 4187 He II 4200

DIB is 4273

Hγ Wavelength (Å) N III 4379 He I 4388 45 DIB is 4428 He I 4438

He I 4471

DIB is 4502 N III 4511 / 15

He II 4542 Si III 4553 Si III 4568 / 75 DIB is 4591 N V 4604 / 20 Si IV 4631 N III 4634 / 41 / 42 Si IV 4654 C III 4647 / 50 / 51

He II 4686

He I 4713 DIB is 4727

DIB is 4762 / 65 / 80

Si III 4813 / 20 / 29

Hβ DIB is 4880 / 87 N III 4905 He I 4922 D h pcrltp sgvnatrtenm.[e h lcrncv electronic the [See name. the after figure.] given a this is classifed of type erroneously stars spectral late-type The for ID. Spectrograms 3.— Fig. 0 1 2 3 4 5 6

0045 504750 4500 4250 4000 Hε

Hδ

Wavelength (Å) Hγ 46 BD +404213F BD +373929F HDE 226144A BD +013974F Tyc 0468 ALS 18890F tr.Tetresaesre yGOS by sorted are targets The stars. O s rino h ora o oo version color a for journal the of ersion − 02112 − 1 F

Hβ i.3—(continued). 3.— Fig. 0 1 2 3 4 5

0045 504750 4500 4250 4000 Hε

Hδ

Wavelength (Å) Hγ 47 CPD BD BD +61100ABG BD +324642AF BD +454132AF − 03 2178K − 61 4623K

Hβ New in paper III 100 New in paper III

Papers I+II Carina 100 Papers I+II

30

10 Cygnus 50 Scorpius Sagittarius

3 Cassiopeia−Perseus Orion−Monoceros

1 Aquila 0 0 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 17 0 30 60 90 120 150 180 210 240 270 300 330 360

Bap l (degrees)

Fig. 4.— [left] Bap and [right] l histograms for the GOSSS new sample in this paper and in papers I and II.

IACOB, and NoMaDS) to obtain their or- features of that plot are real, such as the bits. well known prevalence of some regions of the Galactic plane (Carina and Cygnus are the • Figure 4 [left] shows the Bap distribution of two areas that dominate the O-star popu- the previous and new samples. As expected, lation in the solar neighborhood) and the all new stars have Bap > 8, so our previ- strong effect of foreground extinction in oth- ous claim that the papers I+II sample was ers (the Aquila rift being the most clear one). complete to Bap= 8 is still valid. Our ini- Others are partially created by the differ- tial goal for this paper was to concentrate ent amounts of time we have had allocated on the Bap = 8-11 magnitude range but we in the two hemispheres (so far we have had could not follow that path due to the tech- more time in the north than in the south). nical problems of the Albireo spectrograph It is interesting that the dichotomy between at the 1.5 m OSN telescope and the idiosyn- the first and fourth quadrants on one hand crasies of some time allocation committees. (toward the Galactic center) and the second Strangely enough, in the last years we have and third on the other (away from it) is al- found easier to get observing time for dim ready visible, with more stars in the first stars than for bright ones (even though we case due to the larger stellar densities and have tried both). As a result, we still have disk depths. That is possible despite our many stars to observe in the Bap = 8-11 easier telescope access towards the first three magnitude range, as it is readily apparent quadrants (those completely or partially vis- when comparing Fig. 4 [left] with Fig. 7 in ible from the northern hemisphere), indicat- Ma´ızApell´aniz et al. (2013). We expect to ing the strength of the effect. reverse the situation in the next years, as one of the ultimte goals of GOSSS is to obtain • We have several additional hundreds of non- the massive-star IMF in the solar neighbor- published stars with preliminary O-type hood. classifications already observed with GOSSS and we are currently observing at a rate of • Figure 4 [right] shows the l distribution of ∼200 new ones per year. Our plan is to pub- the previous and new samples. Some of the

48 lish new blocks of O stars similar in quantity SEV-2011-0187 and [b] the Canary Islands Gov- to the one in this paper every approximately ernment under grant PID2 010 119. We would like 2 years. At this rate, we expect to run out to thank Nidia I. Morrell and Miguel Penad´es Or- of O stars with Bap < 14 to observe in the daz for their help in gathering the data for this second and third quadrants in a time scale paper. of 2-3 years. Doing so in the first and fourth quadrants should take significantly longer. REFERENCES • Besides the developments derived from Aharonian, F., Akhperjanian, A. G., Aye, K.-M., GOSSS associated with the stellar prop- et al. 2005, Science, 309, 746 erties (e.g. Arias et al. 2016), we would Aldoretta, E. J., Caballero-Nieves, S. M., Gies, like to point out that GOSSS is turn- D. R., et al. 2015, AJ, 149, 26 ing out to be a treasure trove to study the ISM (Penad´es Ordaz et al. 2011, 2013; Aller, A., Miranda, L. F., Olgu´ın, L., et al. 2015, Ma´ızApell´aniz 2013a, 2015; Ma´ızApell´aniz et al. MNRAS, 446, 317 2014a, 2015c). We are currently working on an analysis of the extinction type and dis- Arias, J. I., et al. 2016, submitted to AJ tribution based on the sample presented in Barb´a, R. H., Gamen, R. C., Arias, J. I., et al. the three GOSSS papers. 2010, in RMxAC, Vol. 38, 30–32 • GOSSS (including some of the new addi- Bassino, L. P., Dessaunet, V. H., Muzzio, J. C., & tions here) is being used as the basis for the Waldhausen, S. 1982, MNRAS, 201, 885 sample selection for the OWN (Barb´aet al. 2010) and IACOB (Sim´on-D´ıaz et al. 2011) Bell, S. A., Hilditch, R. W., & Adamson, A. J. projects. The high-resolution spectra ob- 1987, MNRAS, 225, 961 tained there will be used to derive the prop- erties of the likely single O stars through Bisiacchi, G. F., Lopez, J. A., & Firmani, C. 1982, their quantitative analysis. A&A, 107, 252 Brodskaya, E. S. 1960, IzKry, 24, 160 We thank Brian Skiff for useful comments on Caballero-Nieves, S. M., Nelan, E. P., Gies, D. R., a previous version of this manuscript. J.M.A., et al. 2014, AJ, 147, 40 A.S., and E.J.A. acknowledge support from [a] the Spanish Government Ministerio de Econom´ıa Cannon, A. J., & Mayall, M. W. 1949, AnHar, y Competitividad (MINECO) through grants 112, 1 AYA2010-15081, AYA2010-17631, and AYA2013- Chromey, F. R. 1979, AJ, 84, 534 40 611-P and [b] the Consejer´ıa de Educaci´on of the Junta de Andaluc´ıa through grant P08- Clark, J. S., Najarro, F., Negueruela, I., et al. TIC-4075. J.I.A. and R.H.B. acknowledge sup- 2012, A&A, 541, A145 port from FONDECYT Projects 1140076 and 11121550. I.N. and A.M. acknowledge sup- Clark, J. S., Reig, P., Goodwin, S. P., et al. 2001, port from [a] the Spanish Government Ministe- A&A, 376, 476 rio de Econom´ıa y Competitividad (MINECO) Comer´on, F., & Pasquali, A. 2005, A&A, 430, 541 through grant AYA2012-39364-C02-01/02, [b] the European Union, and [c] the Generalitat —. 2007, A&A, 467, L23 Valenciana through grants ACOMP/2014/129 and BEST/2015/242. A.H. and S.S.-D. ac- —. 2012, A&A, 543, A101 knowledge funding by [a] the Spanish Govern- Conti, P. S. 1973, ApJ, 179, 161 ment Ministerio de Econom´ıa y Competitividad (MINECO) through grants AYA2010-21697-C05- Crampton, D. 1971, AJ, 76, 260 04, AYA2012-39364-C02-01, and Severo Ochoa

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This 2-column preprint was prepared with the AAS LATEX macros v5.2.

53 Table 3 Stars in papers I+II with recently discovered bright companions unresolved in the GOSSS spectra.

Name GOSSSID Ref. New Comments 9 Sgr AB 006.01−01.20 01 S14 B HD 168 112 AB 018.44+01.62 01 S14 B HD 14 633 AaAb 140.78−18.20 01 A15 Ab HD 46 966 AaAb 205.81−00.55 01 S14,A15 Ab σ Ori AaAbB 206.82−17.34 01 H13,S13c Ab B was alreadyin paperI, S15 obtaina moreaccurate spectroscopic orbit. HD 54 662 AB 224.17−00.78 01 S14 B CPD −35 2105 AaAbB 253.64−00.45 01 A15 Ab BwasalreadyconsideredinpaperII. HD 75 759 AB 262.80+01.25 01 S14 B CPD −47 2963 AB 267.98−01.36 01 S14 B HD 93 160 AB 287.44−00.59 01 S14 B WDS 10441−5935 CaCb, HD 93 161 AB is WDS 10441−5935 AB. QZ Car AaAc 287.67−00.94 01 S14 Ac WeusetheWDScomponentnomenclatureinsteadofthat of the paper. HD 93 222 AB 287.74−01.02 01 S14 B HD 96 670 AB 290.20+00.40 01 S14 B HD 97 253 AB 290.79+00.09 01 S14 B HD 101 190 AaAb 294.78−01.49 01 S14 Ab HD 101 131 AB 294.78−01.62 01 S14 B HD 101 545 AaAb 294.88−00.81 01 S14 Ab AseparatespectrumfortheBcomponentwasobtained in paper II. HD 101 413 AB 295.03−01.71 01 S14 B HD 123 590 AB 311.95−01.00 01 S14 B HD 124 314 AaAb 312.67−00.42 01 S14 Ab A separate spectrum for the BaBb component was obtained in paper II. HD 125 206 AB 313.45−00.03 01 S14 B δ Cir AaAbAc 319.69−02.91 01 S14 Ac AaAbisspatiallyunresolvedbutiscataloguedthat way in the WDS. HD 148 937 AaAb 336.37−00.22 01 S14 Ab HD 150 135 AaAb 336.71−01.57 01 S14 Ab WDS 6413−4846 CaCb, HD 150 136 AaAb is WDS 6413−4846 AaAb. HD 150 136 AaAb 336.71−01.57 02 S13a,S13b Ab The inner pair is still unresolved. HD 151 003 AB 342.72+02.41 01 S14 B HD 152 233 AaAb 343.48+01.22 01 S14 Ab WDS 16540−4148 FaFb, HD 152 234 A is WDS 16540−4148 A. HD 152 314 AaAb 343.52+01.14 01 S14 Ab HD 152 247 AaAb 343.61+01.30 01 S14 Ab HD 152 246 AaAb 344.03+01.67 01 S14 Ab HD 152 623 AaAbB 344.62+01.61 01 S14 Ab BwasalreadyconsideredinpaperII. HD 156 738 AB 351.18+00.48 01 S14 B HD 155 806 AB 352.59+02.87 01 S14 B

References. — A15: Aldoretta et al. (2015), H13: Hummel et al. (2013), S13a: Sana et al. (2013), S13b: S´anchez-Berm´udez et al. (2013), S13c: Schaefer (2013), S14: Sana et al. (2014), S15: Sim´on-D´ıaz et al. (2015)

54 Table 4 Spectral reclassifications for stars already present in papers I and II.

Name GOSSS ID RA (J2000) dec (J2000) ST LC Qual. Second.

HD 164 536 GOS 005.96−00.91 01 18:02:38.619 −24:15:19.39 O7.5 V (n) · · · 9 Sgr AB GOS 006.01−01.20 01 18:03:52.446 −24:21:38.64 O4 V ((f)) · · · HD 165 052 GOS 006.12−01.48 01 18:05:10.551 −24:23:54.85 O6 V z O8 Vz HD 168 075 GOS 016.94+00.84 01 18:18:36.043 −13:47:36.46 O6.5 V ((f)) · · · HD 168 076 AB GOS 016.94+00.84 02 18:18:36.421 −13:48:02.38 O4 IV (f) · · · HD 168 112 AB GOS 018.44+01.62 01 18:18:40.868 −12:06:23.39 O5 IV (f) · · · HD 173 010 GOS 023.73−02.49 01 18:43:29.710 −09:19:12.61 O9.7 Ia+ var · · · HDE 344 784 A GOS 059.40−00.15 01 19:43:10.970 +23:17:45.38 O6.5 V ((f))z · · · HD 192 281 GOS 077.12+03.40 01 20:12:33.121 +40:16:05.45 O4.5 IV (n)(f) · · · HDE 229 232 AB GOS 077.40+00.93 01 20:23:59.183 +39:06:15.27 O4 V: n((f)) · · · HD 191 978 GOS 077.87+04.25 01 20:10:58.281 +41:21:09.91 O8 V ··· ··· HD 207 198 GOS 103.14+06.99 01 21:44:53.278 +62:27:38.04 O8.5 II ((f)) · · · BD +60 513 GOS 134.90+00.92 01 02:34:02.530 +61:23:10.87 O7 V n · · · HD 14 434 GOS 135.08−03.82 01 02:21:52.413 +56:54:18.03 O5.5 IV nn(f)p · · · HD 17 520 A GOS 137.22+00.88 01 02:51:14.434 +60:23:09.97 O8 V ··· ··· HD 35 619 GOS 173.04−00.09 01 05:27:36.147 +34:45:18.96 O7.5 V ((f)) · · · HD 36 879 GOS 185.22−05.89 01 05:35:40.527 +21:24:11.72 O7 V (n)((f)) · · · HD 48 099 GOS 206.21+00.80 01 06:41:59.231 +06:20:43.54 O5.5 V ((f))z O9 V HD 46 485 GOS 206.90−01.84 01 06:33:50.957 +04:31:31.62 O7 V ((f))n var? · · · HD 48 279 A GOS 210.41−01.17 01 06:42:40.548 +01:42:58.23 O8.5 V Nstr var? · · · HD 64 315 AB GOS 243.16+00.36 01 07:52:20.284 −26:25:46.69 O5.5 V · · · O7 V CPD -47 2962 GOS 268.00−01.38 01 08:57:51.661 −47:45:43.94 O7 V ((f)) · · · HD 92 206 B GOS 286.22−00.17 02 10:37:22.957 −58:37:23.04 O6 V ((f)) · · · HD 92 206 C GOS 286.22−00.18 01 10:37:18.627 −58:37:41.73 O8 V (n)z B0: V ALS 15 204 GOS 287.40−00.63 02 10:43:41.237 −59:35:48.18 O7.5 V z O9: V HD 93 129 B GOS 287.41−00.57 02 10:43:57.638 −59:32:53.50 O3.5 V ((f))z · · · HD 93 250 AB GOS 287.51−00.54 01 10:44:45.027 −59:33:54.67 O4 IV (fc) · · · V572 Car GOS 287.59−00.69 01 10:44:47.307 −59:43:53.23 O7.5 V (n) B0 V(n) CPD -59 2591 GOS 287.60−00.75 01 10:44:36.688 −59:47:29.63 O8 V z B0.5: V: CPD -59 2626 AB GOS 287.63−00.69 01 10:45:05.794 −59:45:19.60 O7.5 V (n) · · · HD 93 343 GOS 287.64−00.68 01 10:45:12.217 −59:45:00.42 O8 V ··· ··· HD 93 146 A GOS 287.67−01.05 01 10:44:00.158 −60:05:09.86 O7 V ((f)) · · · V662 Car GOS 287.71−00.71 01 10:45:36.318 −59:48:23.37 O5 V (n)z B0: V HD 93 222 AB GOS 287.74−01.02 01 10:44:36.250 −60:05:28.88 O7 V ((f)) · · · HDE 305 525 GOS 287.79−00.71 01 10:46:05.704 −59:50:49.45 O5.5 V ((f))z O7.5 V + B TU Mus GOS 294.81−04.14 01 11:31:10.927 −65:44:32.10 O8 V (n) B0 V(n) δ Cir AaAbAc GOS 319.69−02.91 01 15:16:56.894 −60:57:26.12 O7 IV ((f)) B CPD -41 7721 A GOS 343.44+01.17 01 16:54:06.709 −41:51:07.21 O9.7 V: (n) · · · V1034 Sco GOS 343.48+01.15 01 16:54:19.845 −41:50:09.36 O9.2 IV · · · B1: V HD 152 623 AaAbB GOS 344.62+01.61 01 16:56:15.026 −40:39:35.76 O7 V (n)((f)) · · · HD 156 292 GOS 345.35−03.08 01 17:18:45.814 −42:53:29.92 O9.7 III · · · B ALS 18 770 GOS 348.71−00.79 01 17:19:00.800 −38:49:23.13 O7 V ((f)) · · · HDE 319 703 A GOS 351.03+00.65 01 17:19:46.156 −36:05:52.34 O7 V ((f)) O9.5 V HD 155 806 AB GOS 352.59+02.87 01 17:15:19.247 −33:32:54.30 O7.5 V ((f))(e) · · · HD 158 186 GOS 355.91+01.60 01 17:29:12.925 −31:32:03.44 O9.2 V · · · B1: V

Note.—GOSSS ID is the identification for each star with “GOS” standing for “Galactic O Star”.

55 Table 5 Spectral classifications for new GOSSS stars.

Name GOSSS ID RA (J2000) dec (J2000) ST LC Qual. Second.

ALS 19 618 GOS 015.07−00.70 01 18:20:34.493 −16:10:11.85 O4 V (n)((fc)) · · · BD -16 4826 GOS 015.26−00.73 01 18:21:02.231 −16:01:00.94 O5.5 V ((f))z · · · ALS 4923 GOS 015.70−00.06 01 18:19:28.435 −15:18:46.27 O8.5 V · · · O8.5 V ALS 4626 GOS 015.88+04.22 01 18:04:17.885 −13:06:13.76 ON6 V ((f)) · · · BD -14 5014 GOS 016.65−00.35 01 18:22:22.310 −14:37:08.46 O7.5 V (n)((f)) · · · V479 Sct GOS 016.88−01.29 01 18:26:15.045 −14:50:54.33 ON6 V ((f))z · · · BD -14 5040 GOS 016.90−01.12 01 18:25:38.896 −14:45:05.70 O5.5 V (n)((f)) · · · HD 168 137 AaAb GOS 016.97+00.76 01 18:18:56.189 −13:48:31.08 O8 V z · · · ALS 15 360 GOS 017.00+00.87 01 18:18:37.494 −13:43:39.39 O7 V ((f))z · · · HD 168 504 GOS 017.03+00.35 01 18:20:34.096 −13:57:15.75 O7.5 V (n)z · · · ALS 4880 GOS 018.32+01.87 01 18:17:33.672 −12:05:42.80 O6 V ((f)) · · · HD 168 461 GOS 018.57+01.25 01 18:20:17.179 −12:10:19.19 O7.5 V ((f)) Nstr · · · BD -10 4682 GOS 020.24+01.01 01 18:24:20.651 −10:48:34.29 O7 V n((f)) · · · BD -04 4503 GOS 026.85+01.34 01 18:35:32.534 −04:47:55.39 O7 V ··· ··· HD 175 514 GOS 041.71+03.38 01 18:55:23.124 +09:20:48.07 O7 V (n)((f))z B ALS 18 929 GOS 042.79+10.57 01 18:31:01.379 +13:30:12.85 O9.7 ··· ··· ··· HDE 344 777 GOS 059.41+00.11 01 19:42:11.470 +23:26:00.52 O7.5 V z · · · HDE 344 758 GOS 060.17+00.63 01 19:41:52.721 +24:20:51.07 O8.5 V (n)((f)) · · · HDE 338 931 GOS 061.19−00.14 01 19:47:02.739 +24:50:55.57 O6 III (f) · · · HDE 338 916 GOS 061.47+00.38 01 19:45:42.114 +25:21:16.45 O7.5 V z · · · HDE 227 465 GOS 070.73+01.21 01 20:04:27.225 +33:42:18.40 O7 V ((f)) · · · HDE 227 018 GOS 071.58+02.87 01 19:59:49.103 +35:18:33.53 O6.5 V ((f))z · · · HDE 227 245 GOS 072.17+02.62 01 20:02:21.713 +35:40:29.84 O7 V ((f))z · · · HDE 228 779 GOS 073.18−00.51 01 20:17:54.189 +34:49:02.03 O9 Iab ··· ··· HDE 228 854 GOS 074.54+00.20 01 20:18:47.219 +36:20:26.08 O6 IV n var O5 Vn var ALS 18 707 GOS 074.76+00.62 01 20:17:41.846 +36:45:26.42 O6.5 V ((f))z · · · HD 193 682 GOS 075.92+00.82 01 20:20:08.937 +37:49:51.30 O4.5 IV (f) · · · HD 193 595 GOS 076.86+01.62 01 20:19:31.327 +39:03:26.21 O7 V ((f)) · · · BD +36 4145 GOS 077.45−02.02 01 20:36:18.208 +37:25:02.79 O8.5 V (n) · · · HDE 229 202 GOS 078.19+01.63 01 20:23:22.842 +40:09:22.52 O7.5 V (n)((f)) · · · ALS 11 355 GOS 078.29+00.78 01 20:27:17.572 +39:44:32.55 O8 V (n)((f)) · · · HD 194 649 AB GOS 078.46+01.35 01 20:25:22.124 +40:13:01.07 O6.5 V ((f)) · · · HDE 228 759 GOS 079.01+03.62 01 20:17:07.539 +41:57:26.51 O6.5 V (n)((f))z · · · LS III +41 14 GOS 079.01+03.63 01 20:17:05.515 +41:57:46.89 O9.5 V (n) · · · BD +40 4179 GOS 079.03+01.21 01 20:27:43.617 +40:35:43.53 O8 V z · · · Cyg OB2-B17 GOS 079.84+01.16 01 20:30:27.302 +41:13:25.31 O6 Ia f O9: Ia: Cyg OB2-A24 GOS 080.03+00.30 01 20:34:44.106 +40:51:58.50 O6.5 III (f) · · · 2MASS J20315961+4114504 GOS 080.03+00.94 01 20:31:59.613 +41:14:50.50 O7.5 V z · · · Cyg OB2-A11 GOS 080.08+00.85 01 20:32:31.543 +41:14:08.21 O7 Ib (f) · · · ALS 15 108 AB GOS 080.11+00.67 01 20:33:23.460 +41:09:13.02 O6 IV ((f)) · · · Cyg OB2-5 B GOS 080.12+00.91 02 20:32:22.489 +41:18:19.45 O6.5 Iab fp · · · ALS 15 134 GOS 080.14+00.68 01 20:33:26.749 +41:10:59.51 O8 V z · · · Cyg OB2-22 D GOS 080.14+00.74 02 20:33:10.115 +41:13:10.10 O9.5 V n · · · ALS 15 144 GOS 080.15+00.79 01 20:32:59.643 +41:15:14.67 O9.7 III (n) · · · ALS 15 119 GOS 080.23+00.71 01 20:33:37.001 +41:16:11.30 O9.5 IV (n) · · · Cyg OB2-17 GOS 080.24+00.90 01 20:32:50.011 +41:23:44.71 O8 V ··· ··· Cyg OB2-16 GOS 080.24+00.94 01 20:32:38.575 +41:25:13.76 O7.5 IV (n) · · · Cyg OB2-6 GOS 080.26+00.93 01 20:32:45.447 +41:25:37.50 O8.5 V (n) · · · ALS 15 115 GOS 080.27+00.81 01 20:33:18.046 +41:21:36.90 O8 V ··· ··· ALS 15 111 GOS 080.27+00.88 01 20:32:59.190 +41:24:25.47 O8 V ··· ···

56 Table 5—Continued

Name GOSSS ID RA (J2000) dec (J2000) ST LC Qual. Second.

Cyg OB2-27 AB GOS 080.29+00.66 01 20:33:59.528 +41:17:35.48 O9.7 V (n) O9.7 V:(n) Cyg OB2-73 GOS 080.32+00.60 01 20:34:21.930 +41:17:01.60 O8 V z O8 Vz Cyg OB2-25 A GOS 080.44+00.91 01 20:33:25.539 +41:33:26.74 O8 V z · · · Cyg OB2-10 GOS 080.47+00.85 01 20:33:46.111 +41:33:01.05 O9.7 Iab ··· ··· ALS 15 125 GOS 080.53+00.80 01 20:34:09.519 +41:34:13.69 O9.5 IV: ··· ··· ALS 15 114 GOS 080.54+00.73 01 20:34:29.601 +41:31:45.42 O7.5 V (n)((f)) · · · Cyg OB2-29 GOS 080.55+00.80 01 20:34:13.505 +41:35:03.01 O7.5 V (n)((f))z · · · BD +43 3654 GOS 082.41+02.33 01 20:33:36.080 +43:59:07.41 O4 I f · · · BD +45 3216 A GOS 083.78+03.29 01 20:33:50.366 +45:39:40.95 O5 V ((f))z · · · Bajamar Star GOS 084.81−00.88 01 20:55:51.255 +43:52:24.67 O3.5 III (f*) O8: LS III +46 12 GOS 084.88+03.78 01 20:35:18.566 +46:50:02.90 O4.5 IV (f) · · · LS III +46 11 GOS 084.88+03.81 01 20:35:12.642 +46:51:12.12 O3.5 I f* O3.5 If* ALS 11 761 GOS 088.81−01.12 01 21:12:00.455 +46:41:51.31 O9.2 II ··· ··· ALS 12 050 GOS 101.08+02.47 01 21:55:15.291 +57:39:45.66 O5 V ((f)) · · · BD +55 2722 A GOS 102.81−00.67 01 22:18:58.629 +56:07:23.47 O8 V z · · · BD +55 2722 C GOS 102.81−00.67 02 22:18:59.876 +56:07:18.92 O7 V (n)z B BD +55 2722 B GOS 102.81−00.67 03 22:18:58.832 +56:07:23.47 O9.5 V ··· ··· ALS 12 320 GOS 102.98−00.76 01 22:20:21.783 +56:08:52.21 O7 IV ((f)) · · · ALS 12 370 GOS 103.05−01.41 01 22:23:17.417 +55:38:02.31 O6.5 V nn((f)) · · · ALS 12 619 GOS 107.18−00.95 01 22:47:50.595 +58:05:12.39 O7 V ((f))z · · · BD +55 2840 GOS 107.30−02.92 01 22:55:08.492 +56:22:58.88 O7.5 V (n) · · · ALS 12 688 GOS 107.42−02.87 01 22:55:44.944 +56:28:36.70 O5.5 V (n)((fc)) B BD +62 2078 GOS 107.45+05.02 01 22:25:33.579 +63:25:02.62 O7 V ((f))z · · · HD 213 023 A GOS 107.73+05.20 01 22:26:52.362 +63:43:04.87 O7.5 V z · · · ALS 12 749 GOS 108.54−02.74 01 23:02:44.556 +57:03:50.21 O9 V ··· ··· Sh 2-158 2 GOS 111.53+00.82 01 23:13:30.243 +61:30:10.34 O9.5: V · · · B0.5: V Sh 2-158 1 GOS 111.53+00.82 02 23:13:34.435 +61:30:14.73 O3.5 V ((f*)) O9.5: V BD +60 2635 GOS 115.90−01.16 01 23:53:05.205 +60:54:44.62 O6 V ((f)) · · · BD +66 1661 GOS 117.81+05.22 01 23:57:32.603 +67:33:15.28 O9.2 V ··· ··· V747 Cep GOS 118.20+05.09 01 00:01:46.870 +67:30:25.13 O5.5 V (n)((f)) · · · BD +66 1675 GOS 118.21+04.99 01 00:02:10.287 +67:24:32.22 O7.5 V z · · · BD +66 1674 GOS 118.22+05.01 01 00:02:10.236 +67:25:45.21 O9.7 IV: ··· ··· Tyc 4026-00424-1 GOS 118.23+05.01 01 00:02:19.027 +67:25:38.55 O7 V ((f))z · · · ALS 6351 GOS 122.57+00.12 01 00:48:12.548 +62:59:24.84 O7 V z · · · BD +60 134 GOS 123.50−01.11 01 00:56:14.216 +61:45:36.91 O5.5 V (n)((f)) · · · HD 5689 GOS 123.86+00.75 01 00:59:47.589 +63:36:28.27 O7 V n((f)) · · · ALS 6967 GOS 132.94−01.39 01 02:12:29.974 +59:54:04.12 O8 V · · · B0: V BD +61 411 A GOS 133.84+01.17 01 02:26:34.379 +62:00:42.32 O6.5 V ((f))z · · · ALS 7833 GOS 146.25+03.12 01 03:59:07.494 +57:14:11.69 O8 V z · · · MY Cam GOS 146.27+03.14 01 03:59:18.290 +57:14:13.72 O5.5 V (n) O6.5 V(n) BD +50 886 GOS 150.60−00.94 01 04:03:20.736 +51:18:52.46 O4 V ((fc)) · · · BD +52 805 GOS 151.26+01.79 01 04:18:35.640 +52:51:54.21 O8 V (n) · · · ALS 8272 GOS 168.75+01.00 01 05:20:00.634 +38:54:43.54 O7 V ((f)) B0 III-V ALS 8294 GOS 173.61−01.72 01 05:22:39.690 +33:22:18.23 O7 V (n)z · · · ALS 19 265 GOS 186.10+06.56 01 06:24:59.866 +26:49:19.41 O4.5 V ((c))z · · · HDE 256 725 A GOS 192.32+03.36 01 06:25:01.300 +19:50:56.07 O5 V ((fc)) · · · HDE 256 725 B GOS 192.32+03.36 02 06:25:01.900 +19:50:54.52 O9.5 V ··· ··· Tyc 0737-01170-1 GOS 201.61+01.64 01 06:36:29.003 +10:49:20.73 O7 V z · · · ALS 85 GOS 218.82−04.57 01 06:45:48.800 −07:18:46.63 O7.5 V ··· ··· ALS 207 GOS 231.49−04.40 01 07:09:55.206 −18:30:07.88 O6.5 V ((f)) · · ·

57 Table 5—Continued

Name GOSSS ID RA (J2000) dec (J2000) ST LC Qual. Second.

BD -15 1909 GOS 232.31+01.94 01 07:34:58.463 −16:14:23.22 O6.5 V ((f))z · · · ALS 458 GOS 234.28−00.50 01 07:30:01.272 −19:08:34.98 O6.5 V ((f))z · · · V441 Pup GOS 240.28−04.05 01 07:28:53.586 −26:06:28.89 O5: V e · · · CPD -26 2704 GOS 243.14+00.44 01 07:52:36.593 −26:22:41.99 O7 V (n) · · · V467 Vel GOS 265.20−02.18 01 08:43:49.809 −46:07:08.78 O6.5 V (n)((f)) · · · CPD -49 2322 GOS 271.65−00.70 01 09:15:52.787 −50:00:43.82 O7.5 V ((f)) · · · HD 90 273 GOS 284.18−00.25 01 10:23:44.454 −57:38:31.55 ON7 V ((f)) · · · THA 35-II-42 GOS 284.52−00.24 01 10:25:56.505 −57:48:43.50 O2 I f*/WN5 · · · HD 89 625 GOS 284.81−02.37 01 10:18:58.251 −59:46:04.30 ON9.2 IV n · · · 2MASS J10224377-5930182 GOS 285.06−01.89 01 10:22:43.774 −59:30:18.22 O8 V (n) · · · 2MASS J10224096-5930305 GOS 285.06−01.90 01 10:22:40.961 −59:30:30.58 O7 V ((f))z · · · ALS 18 551 GOS 289.73−01.26 01 10:58:17.678 −61:12:03.48 O4.5 V (n)z O4.5 V(n)z 2MASS J10584671-6105512 GOS 289.74−01.14 01 10:58:46.716 −61:05:51.22 O8 Iab f · · · ALS 18 553 GOS 289.74−01.18 01 10:58:37.773 −61:08:00.35 O6 II (f) · · · 2MASS J10583238-6110565 GOS 289.75−01.23 01 10:58:32.389 −61:10:56.50 O5 V ((f)) O7 V((f)) THA 35-II-153 GOS 289.79−01.18 01 10:59:00.805 −61:08:50.24 O3.5 I f*/WN7 · · · HD 97 966 GOS 290.96+01.20 01 11:15:11.779 −59:24:58.28 O7 V ((f))z · · · HD 97 319 GOS 291.12−00.57 01 11:11:06.156 −61:07:04.56 O7.5 IV ((f)) · · · EM Car GOS 291.22−00.50 01 11:12:04.503 −61:05:42.94 O7.5 V ((f)) O7.5 V((f)) NGC 3603 HST-51 GOS 291.62−00.52 15 11:15:07.498 −61:15:46.35 O5.5 V (n) · · · NGC 3603 HST-48 GOS 291.62−00.53 02 11:15:08.712 −61:15:59.95 O3.5 I f* · · · NGC 3603 HST-24 GOS 291.62−00.53 03 11:15:09.353 −61:16:02.07 O4 IV (f) · · · NGC 3603 MTT 25 GOS 291.63−00.52 01 11:15:11.317 −61:15:55.63 O5 V (n) · · · HD 99 546 GOS 292.33+01.68 01 11:26:36.905 −59:26:13.61 O7.5 V ((f)) Nstr · · · HD 110 360 GOS 301.80+02.20 01 12:42:12.700 −60:39:08.71 ON7 V ··· ··· CPD -61 3973 GOS 309.13−00.20 01 13:45:21.103 −62:25:35.37 O7.5 V ((f)) · · · HD 122 313 GOS 311.18−00.54 01 14:03:12.987 −62:15:38.60 O8.5 V ··· ··· ALS 17 591 GOS 320.32−01.16 01 15:13:55.206 −59:07:51.61 O5: · · · n(f)p · · · ALS 3386 GOS 326.31+00.74 01 15:42:12.037 −54:11:21.27 O6 Ia f · · · ALS 18 049 GOS 326.73+00.77 01 15:44:20.206 −53:54:41.31 O9 V ··· ··· Muzzio III-9 GOS 327.39−00.62 01 15:53:48.597 −54:35:10.64 O8 Ib (f) · · · HD 145 217 GOS 332.29+00.77 01 16:12:00.298 −50:18:20.48 O8 V ··· ··· HD 144 647 GOS 332.45+01.58 01 16:09:16.197 −49:36:21.75 O8.5 V (n) · · · HDE 328 209 AB GOS 338.49+02.85 01 16:29:19.165 −44:28:14.27 ON9 Ib-Ia p · · · HDE 329 100 A GOS 340.86−01.05 01 16:54:42.304 −45:15:14.80 O8 V (n) · · · HDE 326 775 GOS 345.01−00.30 01 17:05:31.316 −41:31:20.12 O6.5 V (n)((f))z · · · ALS 18 769 GOS 348.67−00.79 01 17:18:53.372 −38:51:13.23 O6 II (f) · · · HDE 323 110 GOS 349.65−00.67 01 17:21:15.794 −37:59:09.58 ON9 Ia ··· ··· Tyc 7370-00460-1 GOS 352.57+02.11 01 17:18:15.396 −34:00:05.94 O6 V ((f)) O8 V ALS 19 693 GOS 353.07+00.64 01 17:25:29.167 −34:25:15.74 O6 V n((f)) · · · Pismis 24-15 GOS 353.10+00.91 01 17:24:28.952 −34:14:50.68 O7.5 V z · · · ALS 19 692 GOS 353.11+00.65 01 17:25:34.213 −34:23:11.68 O5.5 IV (f) · · ·

Note.—GOSSS ID is the identification for each star with “GOS” standing for “Galactic O Star”.

58 Table 6 Spectral classifications for late-type stars erroneously classifed as O stars.

Name RA (J2000) dec (J2000) Simbad GOSSS Ref. Fixed? Comment

ALS 18 890 19:35:23.587 −16:19:46.78 O+. . . F None No Tyc 0468-02112-1 19:16:44.466 +02:28:41.60 O. . . F None Yes Currently K86 given as reference for an F? spectral type. BD +01 3974 19:22:01.484 +02:12:01.90 O F K86 No HDE 226 144 19:50:59.376 +36:00:03.24 O9 V A M80 No BD +37 3929 20:25:20.022 +37:42:23.25 O8f F H56 No Confusion with BD +37 3927. BD +40 4213 20:31:46.006 +41:17:27.07 O9.5 I F M91 No Not in the original reference, likely transcription error in SIMBAD. BD +45 4132 A 23:04:14.816 +46:36:33.63 O F None Yes BD +32 4642 A 23:25:38.697 +33:26:16.94 O F None Yes BD +61 100 AB 00:30:32.445 +62:34:00.93 O/B2 G R89 No A different reference is given now but the link is broken. BD -03 2178 08:02:10.340 −04:01:36.39 O5 K M76 Yes Confusion with BD -03 2179, a sdO. CPD −61 4623 14:35:36.520 −61:34:12.77 O K None Yes

59 References. — B60:Brodskaya (1960), H56:Hiltner & Johnson (1956), K86:Kelly & Kilkenny (1986), M76: MacConnell & Bidelman (1976), M80:Mikolajewska & Mikolajewski (1980), M91:Massey & Thompson (1991), R89:Radoslavova (1989)